Performance information

• X-Ray Imaging and Spectroscopy Mission
  Makoto Tashiro; Richard Kelley; Shin Watanabe; Hironori Maejima; Lillian Reichenthal; Kenichi Toda; Leslie Hartz; Andrea Santovincenzo; Kyoko Matsushita; Hiroya Yamaguchi; Robert Petre; Brian Williams; Matteo Guainazzi; Elisa Costantini; Yoh Takei; Yoshitaka Ishisaki; Ryuichi Fujimoto; Joy Henegar-Leon; Gary Sneiderman; Hiroshi Tomida; Koji Mori; Hiroshi Nakajima; Yukikatsu Terada; Matthew Holland; Michael Loewenstein; Eric Miller; Makoto Sawada; Timothy Kallman; Jelle Kaastra; Chris Done; Teruaki Enoto; Aya Bamba; Lia Corrales; Yoshihiro Ueda; Erin Kara; Irina Zhuravleva; Yutaka Fujita; Yoshitaka Arai; Marc Audard; Hisamitsu Awaki; Ralf Ballhausen; Chris Baluta; Nobutaka Bando; Ehud Behar; Thomas Bialas; Rozenn Boissay-Malaquin; Laura Brenneman; Gregory V Brown; Meng Chiao; Renata Cumbee; Cor de Vries; Jan-Willem den Herder; María Díaz Trigo; Michael DiPirro; Tadayasu Dotani; Jacobo Ebrero Carrero; Ken Ebisawa; Megan Eckart; Dominique Eckert; Satoshi Eguchi; Yuichiro Ezoe; Carlo Ferrigno; Adam Foster; Yasushi Fukazawa; Kotaro Fukushima; Akihiro Furuzawa; Luigi Gallo; Javier Garcia Martinez; Nathalie Gorter; Martin Grim; Liyi Gu; Kouichi Hagino; Kenji Hamaguchi; Isamu Hatsukade; Katsuhiro Hayashi; Takayuki Hayashi; Natalie Hell; Edmund Hodges-Kluck; Takafumi Horiuchi; Ann Hornschemeier; Akio Hoshino; Yuto Ichinohe; Chisato Ikuta; Ryo Iizuka; Daiki Ishi; Manabu Ishida; Naoki Ishihama; Kumi Ishikawa; Kosei Ishimura; Tess Jaffe; Satoru Katsuda; Yoshiaki Kanemaru; Steven Kenyon; Caroline Kilbourne; Mark Kimball; Shunji Kitamoto; Shogo Kobayashi; Takayoshi Kohmura; Aya Kubota; Maurice Leutenegger; Yoshitomo Maeda; Maxim Markevitch; Hironori Matsumoto; Keiichi Matsuzaki; Dan McCammon; Brian McLaughlin; Brian McNamara; Francois Mernier; Joseph Miko; Jon Miller; Kenji Minesugi; Shinji Mitani; Ikuyuki Mitsuishi; Misaki Mizumoto; Tsunefumi Mizuno; Koji Mukai; Hiroshi Murakami; Richard Mushotzky; Kazuhiro Nakazawa; Chikara Natsukari; Jan-Uwe Ness; Kenichiro Nigo; Mari Nishiyama; Kumiko Nobukawa; Masayoshi Nobukawa; Hirofumi Noda; Hirokazu Odaka; Mina Ogawa; Shoji Ogawa; Anna Ogorzalek; Takashi Okajima; Atsushi Okamoto; Naomi Ota; Masanobu Ozaki; Stephane Paltani; Paul Plucinsky; F Scott Porter; Katja Pottschmidt; Jose Antonio Quero; Takahiro Sasaki; Kosuke Sato; Rie Sato; Toshiki Sato; Yoichi Sato; Hiromi Seta; Maki Shida; Megumi Shidatsu; Shuhei Shigeto; Russel Shipman; Keisuke Shinozaki; Peter Shirron; Aurora Simionescu; Randall Smith; Yang Soong; Hiromasa Suzuki; Andrew Szymkowiak; Hiromitsu Takahashi; Mai Takeo; Toru Tamagawa; Keisuke Tamura; Takaaki Tanaka; Atsushi Tanimoto; Yuichi Terashima; Yohko Tsuboi; Masahiro Tsujimoto; Hiroshi Tsunemi; Takeshi Tsuru; Hiroyuki Uchida; Nagomi Uchida; Yuusuke Uchida; Hideki Uchiyama; Shinichiro Uno; Jacco Vink; Michael Witthoeft; Rob Wolfs; Satoshi Yamada; Shinya Yamada; Kazutaka Yamaoka; Noriko Yamasaki; Makoto Yamauchi; Shigeo Yamauchi; Keiichi Yanagase; Tahir Yaqoob; Susumu Yasuda; Tomokage Yoneyama; Tessei Yoshida; Miohoko Yukita
  Publications of the Astronomical Society of Japan, Apr. 2025, [Reviewed], [Lead, Corresponding]
  Abstract
  
  The X-Ray Imaging and Spectroscopy Mission (XRISM) is a joint mission between the Japan Aerospace Exploration Agency (JAXA) and the National Aeronautics and Space Administration (NASA) in collaboration with the European Space Agency (ESA). In addition to the three space agencies, universities and research institutes from Japan, North America, and Europe have joined to contribute to developing satellite and onboard instruments, data-processing software, and the scientific observation program. XRISM is the successor to the ASTRO-H (Hitomi) mission, which ended prematurely in 2016. Its primary science goal is to examine astrophysical problems with precise, high-resolution X-ray spectroscopy. XRISM promises to discover new horizons in X-ray astronomy. It carries a 6 × 6 pixelized X-ray microcalorimeter on the focal plane of an X-ray mirror assembly (Resolve) and a co-aligned X-ray CCD camera (Xtend) that covers the same energy band over a large field of view. XRISM utilizes the Hitomi heritage, but all designs were reviewed. The attitude and orbit control system was improved in hardware and software. The spacecraft was launched from the JAXA Tanegashima Space Center on 2023 September 6 (UTC). During the in-orbit commissioning phase, the onboard components were activated. Although the gate valve protecting the Resolve sensor with a thin beryllium X-ray entrance window was not yet opened, scientific observation started in 2024 February with the planned performance verification observation program. The nominal observation program commenced with the following guest observation program beginning in 2024 September.
  Oxford University Press (OUP), English, Scientific journal
  DOI：https://doi.org/10.1093/pasj/psaf023
  DOI ID：10.1093/pasj/psaf023, ISSN：0004-6264, eISSN：2053-051X
• The bulk motion of gas in the core of the Centaurus galaxy cluster
  Marc Audard; Hisamitsu Awaki; Ralf Ballhausen; Aya Bamba; Ehud Behar; Rozenn Boissay-Malaquin; Laura Brenneman; Gregory V. Brown; Lia Corrales; Elisa Costantini; Renata Cumbee; Chris Done; Tadayasu Dotani; Ken Ebisawa; Megan E. Eckart; Dominique Eckert; Teruaki Enoto; Satoshi Eguchi; Yuichiro Ezoe; Adam Foster; Ryuichi Fujimoto; Yutaka Fujita; Yasushi Fukazawa; Kotaro Fukushima; Akihiro Furuzawa; Luigi Gallo; Javier A. García; Liyi Gu; Matteo Guainazzi; Kouichi Hagino; Kenji Hamaguchi; Isamu Hatsukade; Katsuhiro Hayashi; Takayuki Hayashi; Natalie Hell; Edmund Hodges-Kluck; Ann Hornschemeier; Yuto Ichinohe; Manabu Ishida; Kumi Ishikawa; Yoshitaka Ishisaki; Jelle Kaastra; Timothy Kallman; Erin Kara; Satoru Katsuda; Yoshiaki Kanemaru; Richard Kelley; Caroline Kilbourne; Shunji Kitamoto; Shogo Kobayashi; Takayoshi Kohmura; Aya Kubota; Maurice Leutenegger; Michael Loewenstein; Yoshitomo Maeda; Maxim Markevitch; Hironori Matsumoto; Kyoko Matsushita; Dan McCammon; Brian McNamara; François Mernier; Eric D. Miller; Jon M. Miller; Ikuyuki Mitsuishi; Misaki Mizumoto; Tsunefumi Mizuno; Koji Mori; Koji Mukai; Hiroshi Murakami; Richard Mushotzky; Hiroshi Nakajima; Kazuhiro Nakazawa; Jan-Uwe Ness; Kumiko Nobukawa; Masayoshi Nobukawa; Hirofumi Noda; Hirokazu Odaka; Shoji Ogawa; Anna Ogorzalek; Takashi Okajima; Naomi Ota; Stephane Paltani; Robert Petre; Paul Plucinsky; Frederick Scott Porter; Katja Pottschmidt; Kosuke Sato; Toshiki Sato; Makoto Sawada; Hiromi Seta; Megumi Shidatsu; Aurora Simionescu; Randall Smith; Hiromasa Suzuki; Andrew Szymkowiak; Hiromitsu Takahashi; Mai Takeo; Toru Tamagawa; Keisuke Tamura; Takaaki Tanaka; Atsushi Tanimoto; Makoto Tashiro; Yukikatsu Terada; Yuichi Terashima; María Díaz Trigo; Yohko Tsuboi; Masahiro Tsujimoto; Hiroshi Tsunemi; Takeshi G. Tsuru; Hiroyuki Uchida; Nagomi Uchida; Yuusuke Uchida; Hideki Uchiyama; Yoshihiro Ueda; Shinichiro Uno; Jacco Vink; Shin Watanabe; Brian J. Williams; Satoshi Yamada; Shinya Yamada; Hiroya Yamaguchi; Kazutaka Yamaoka; Noriko Y. Yamasaki; Makoto Yamauchi; Shigeo Yamauchi; Tahir Yaqoob; Tomokage Yoneyama; Tessei Yoshida; Mihoko Yukita; Irina Zhuravleva; Marie Kondo; Norbert Werner; Tomáš Plšek; Ming Sun; Kokoro Hosogi; Anwesh Majumder
  Nature, Volume：638, Number：8050, First page：365, Last page：369, Feb. 2025, [Reviewed]
  Springer Science and Business Media LLC, Scientific journal
  DOI：https://doi.org/10.1038/s41586-024-08561-z
  DOI ID：10.1038/s41586-024-08561-z, ISSN：0028-0836, eISSN：1476-4687
• Overionized plasma in the supernova remnant Sagittarius A East anchored by XRISM observations
  Marc Audard; Hisamitsu Awaki; Ralf Ballhausen; Aya Bamba; Ehud Behar; Rozenn Boissay-Malaquin; Laura Brenneman; Gregory V Brown; Lia Corrales; Elisa Costantini; Renata Cumbee; Maria Diaz-Trigo; Chris Done; Tadayasu Dotani; Ken Ebisawa; Megan Eckart; Dominique Eckert; Teruaki Enoto; Satoshi Eguchi; Yuichiro Ezoe; Adam Foster; Ryuichi Fujimoto; Yutaka Fujita; Yasushi Fukazawa; Kotaro Fukushima; Akihiro Furuzawa; Luigi Gallo; Javier A García; Liyi Gu; Matteo Guainazzi; Kouichi Hagino; Kenji Hamaguchi; Isamu Hatsukade; Katsuhiro Hayashi; Takayuki Hayashi; Natalie Hell; Edmund Hodges-Kluck; Ann Hornschemeier; Yuto Ichinohe; Manabu Ishida; Kumi Ishikawa; Yoshitaka Ishisaki; Jelle Kaastra; Timothy Kallman; Erin Kara; Satoru Katsuda; Yoshiaki Kanemaru; Richard Kelley; Caroline Kilbourne; Shunji Kitamoto; Shogo Kobayashi; Takayoshi Kohmura; Aya Kubota; Maurice Leutenegger; Michael Loewenstein; Yoshitomo Maeda; Maxim Markevitch; Hironori Matsumoto; Kyoko Matsushita; Dan McCammon; Brian McNamara; François Mernier; Eric D Miller; Jon M Miller; Ikuyuki Mitsuishi; Misaki Mizumoto; Tsunefumi Mizuno; Koji Mori; Koji Mukai; Hiroshi Murakami; Richard Mushotzky; Hiroshi Nakajima; Kazuhiro Nakazawa; Jan-Uwe Ness; Kumiko Nobukawa; Masayoshi Nobukawa; Hirofumi Noda; Hirokazu Odaka; Shoji Ogawa; Anna Ogorzalek; Takashi Okajima; Naomi Ota; Stephane Paltani; Robert Petre; Paul Plucinsky; Frederick Scott Porter; Katja Pottschmidt; Kosuke Sato; Toshiki Sato; Makoto Sawada; Hiromi Seta; Megumi Shidatsu; Aurora Simionescu; Randall Smith; Hiromasa Suzuki; Andrew Szymkowiak; Hiromitsu Takahashi; Mai Takeo; Toru Tamagawa; Keisuke Tamura; Takaaki Tanaka; Atsushi Tanimoto; Makoto Tashiro; Yukikatsu Terada; Yuichi Terashima; Yohko Tsuboi; Masahiro Tsujimoto; Hiroshi Tsunemi; Takeshi G Tsuru; Hiroyuki Uchida; Nagomi Uchida; Yuusuke Uchida; Hideki Uchiyama; Yoshihiro Ueda; Shinichiro Uno; Jacco Vink; Shin Watanabe; Brian J Williams; Satoshi Yamada; Shinya Yamada; Hiroya Yamaguchi; Kazutaka Yamaoka; Noriko Yamasaki; Makoto Yamauchi; Shigeo Yamauchi; Tahir Yaqoob; Tomokage Yoneyama; Tessei Yoshida; Mihoko Yukita; Irina Zhuravleva; Q Daniel Wang; Yuki Amano; Kojiro Tanaka; Takuto Narita; Yuken Ohshiro; Anje Yoshimoto; Yuma Aoki; Mayura Balakrishnan
  Publications of the Astronomical Society of Japan, Volume：77, Number：1, First page：L1, Last page：L8, Dec. 2024, [Reviewed]
  Abstract
  
  Sagittarius A East is a supernova remnant with a unique surrounding environment, as it is located in the immediate vicinity of the supermassive black hole at the Galactic center, Sagittarius A$^{*}$. The X-ray emission of the remnant is suspected to show features of overionized plasma, which would require peculiar evolutionary paths. We report on the first observation of Sagittarius A East with the X-Ray Imaging and Spectroscopy Mission (XRISM). Equipped with a combination of a high-resolution microcalorimeter spectrometer and a large field-of-view CCD imager, we for the first time resolved the Fe xxv K-shell lines into fine structure lines and measured the forbidden-to-resonance intensity ratio to be $1.39 \pm 0.12$, which strongly suggests the presence of overionized plasma. We obtained a reliable constraint on the ionization temperature just before the transition into the overionization state, of $\gt\! 4\:$keV. The recombination timescale was constrained to be $\lt\! 8 \times 10^{11} \:$cm$^{-3}\:$s. The small velocity dispersion of $109 \pm 6\:$km$\:$s$^{-1}$ indicates a low Fe ion temperature $\lt\! 8\:$keV and a small expansion velocity $\lt\! 200\:$km$\:$s$^{-1}$. The high initial ionization temperature and small recombination timescale suggest that either rapid cooling of the plasma via adiabatic expansion from dense circumstellar material or intense photoionization by Sagittarius A$^{*}$ in the past may have triggered the overionization.
  Oxford University Press (OUP), Scientific journal
  DOI：https://doi.org/10.1093/pasj/psae111
  DOI ID：10.1093/pasj/psae111, ISSN：0004-6264, eISSN：2053-051X
• The XRISM/Resolve View of the Fe K Region of Cyg X-3
  Marc Audard; Hisamitsu Awaki; Ralf Ballhausen; Aya Bamba; Ehud Behar; Rozenn Boissay-Malaquin; Laura Brenneman; Gregory V. Brown; Lia Corrales; Elisa Costantini; Renata Cumbee; María Díaz Trigo; Chris Done; Tadayasu Dotani; Ken Ebisawa; Megan E. Eckart; Dominique Eckert; Satoshi Eguchi; Teruaki Enoto; Yuichiro Ezoe; Adam Foster; Ryuichi Fujimoto; Yutaka Fujita; Yasushi Fukazawa; Kotaro Fukushima; Akihiro Furuzawa; Luigi Gallo; Javier A. García; Liyi Gu; Matteo Guainazzi; Kouichi Hagino; Kenji Hamaguchi; Isamu Hatsukade; Katsuhiro Hayashi; Takayuki Hayashi; Natalie Hell; Edmund Hodges-Kluck; Ann Hornschemeier; Yuto Ichinohe; Manabu Ishida; Kumi Ishikawa; Yoshitaka Ishisaki; Jelle Kaastra; Timothy Kallman; Erin Kara; Satoru Katsuda; Yoshiaki Kanemaru; Richard Kelley; Caroline Kilbourne; Shunji Kitamoto; Shogo Kobayashi; Takayoshi Kohmura; Aya Kubota; Maurice Leutenegger; Michael Loewenstein; Yoshitomo Maeda; Maxim Markevitch; Hironori Matsumoto; Kyoko Matsushita; Dan McCammon; Brian McNamara; François Mernier; Eric D. Miller; Jon M. Miller; Ikuyuki Mitsuishi; Misaki Mizumoto; Tsunefumi Mizuno; Koji Mori; Koji Mukai; Hiroshi Murakami; Richard Mushotzky; Hiroshi Nakajima; Kazuhiro Nakazawa; Jan-Uwe Ness; Kumiko Nobukawa; Masayoshi Nobukawa; Hirofumi Noda; Hirokazu Odaka; Shoji Ogawa; Anna Ogorzalek; Takashi Okajima; Naomi Ota; Stephane Paltani; Robert Petre; Paul Plucinsky; Frederick S. Porter; Katja Pottschmidt; Kosuke Sato; Toshiki Sato; Makoto Sawada; Hiromi Seta; Megumi Shidatsu; Aurora Simionescu; Randall Smith; Hiromasa Suzuki; Andrew Szymkowiak; Hiromitsu Takahashi; Mai Takeo; Toru Tamagawa; Keisuke Tamura; Takaaki Tanaka; Atsushi Tanimoto; Makoto Tashiro; Yukikatsu Terada; Yuichi Terashima; Yohko Tsuboi; Masahiro Tsujimoto; Hiroshi Tsunemi; Takeshi Tsuru; Hiroyuki Uchida; Nagomi Uchida; Yuusuke Uchida; Hideki Uchiyama; Yoshihiro Ueda; Shinichiro Uno; Jacco Vink; Shin Watanabe; Brian J. Williams; Satoshi Yamada; Shinya Yamada; Hiroya Yamaguchi; Kazutaka Yamaoka; Noriko Yamasaki; Makoto Yamauchi; Shigeo Yamauchi; Tahir Yaqoob; Tomokage Yoneyama; Tessei Yoshida; Mihoko Yukita; Irina Zhuravleva; Ryota Tomaru; Tasuku Hayashi; Tomohiro Hakamata; Daiki Miura; Karri Koljonen; Mike McCollough
  The Astrophysical Journal Letters, Volume：977, Number：2, First page：L34, Last page：L34, Dec. 2024, [Reviewed]
  Abstract
  
  The X-ray binary system Cygnus X-3 (4U 2030+40, V1521 Cyg) is luminous but enigmatic owing to the high intervening absorption. High-resolution X-ray spectroscopy uniquely probes the dynamics of the photoionized gas in the system. In this Letter, we report on an observation of Cyg X-3 with the XRISM/Resolve spectrometer, which provides unprecedented spectral resolution and sensitivity in the 2–10 keV band. We detect multiple kinematic and ionization components in absorption and emission whose superposition leads to complex line profiles, including strong P Cygni profiles on resonance lines. The prominent Fe xxv Heα and Fe xxvi Lyα emission complexes are clearly resolved into their characteristic fine-structure transitions. Self-consistent photoionization modeling allows us to disentangle the absorption and emission components and measure the Doppler velocity of these components as a function of binary orbital phase. We find a significantly higher velocity amplitude for the emission lines than for the absorption lines. The absorption lines generally appear blueshifted by ∼−500–600 km s⁻¹. We show that the wind decomposes naturally into a relatively smooth and large-scale component, perhaps associated with the background wind itself, plus a turbulent, denser structure located close to the compact object in its orbit.
  American Astronomical Society, Scientific journal
  DOI：https://doi.org/10.3847/2041-8213/ad8ed0
  DOI ID：10.3847/2041-8213/ad8ed0, ISSN：2041-8205, eISSN：2041-8213
• X‐Raying Neutral Density Disturbances in the Mesosphere and Lower Thermosphere Induced by the 2022 Hunga‐Tonga Volcano Eruption‐Explosion
  Satoru Katsuda; Hiroyuki Shinagawa; Hitoshi Fujiwara; Hidekatsu Jin; Yasunobu Miyoshi; Yoshizumi Miyoshi; Yuko Motizuki; Motoki Nakajima; Kazuhiro Nakazawa; Kumiko K. Nobukawa; Yuichi Otsuka; Atsushi Shinbori; Takuya Sori; Chihiro Tao; Makoto S. Tashiro; Yuuki Wada; Takaya Yamawaki
  Geophysical Research Letters, Volume：51, Number：20, Oct. 2024, [Reviewed]
  Abstract
  
  We present X‐ray observations of the upper atmospheric density disturbance caused by the explosive eruption of the Hunga Tonga‐Hunga Ha'apai (HTHH) volcano on 15 January 2022. From 14 January to 16 January, the Chinese X‐ray astronomy satellite, Insight‐HXMT, was observing the supernova remnant Cassiopeia A. The X‐ray data obtained during Earth's atmospheric occultations allowed us to measure neutral densities in the altitude range of 90–150 km. The density profiles above 110 km altitude obtained before the major eruption are in reasonable agreement with expectations by both GAIA and NRLMSIS 2.0 models. In contrast, after the HTHH eruption, a severe density depletion was found up to 1,000 km away from the epicenter, and a relatively weak depletion extending up to km for over 8 hr after the eruption. In addition, density profiles showed wavy structures with a typical length scale of either 20 km (vertical) or 1,000 km (horizontal). This may be caused by Lamb waves or gravity waves triggered by the volcanic eruption.
  American Geophysical Union (AGU), Scientific journal
  DOI：https://doi.org/10.1029/2024gl112025
  DOI ID：10.1029/2024gl112025, ISSN：0094-8276, eISSN：1944-8007, ORCID：166445828
• The XRISM first-light observation: Velocity structure and thermal properties of the supernova remnant N 132D
  Marc Audard; Hisamitsu Awaki; Ralf Ballhausen; Aya Bamba; Ehud Behar; Rozenn Boissay-Malaquin; Laura Brenneman; Gregory V Brown; Lia Corrales; Elisa Costantini; Renata Cumbee; Maria Diaz-Trigo; Chris Done; Tadayasu Dotani; Ken Ebisawa; Megan Eckart; Dominique Eckert; Teruaki Enoto; Satoshi Eguchi; Yuichiro Ezoe; Adam Foster; Ryuichi Fujimoto; Yutaka Fujita; Yasushi Fukazawa; Kotaro Fukushima; Akihiro Furuzawa; Luigi Gallo; Javier A García; Liyi Gu; Matteo Guainazzi; Kouichi Hagino; Kenji Hamaguchi; Isamu Hatsukade; Katsuhiro Hayashi; Takayuki Hayashi; Natalie Hell; Edmund Hodges-Kluck; Ann Hornschemeier; Yuto Ichinohe; Manabu Ishida; Kumi Ishikawa; Yoshitaka Ishisaki; Jelle Kaastra; Timothy Kallman; Erin Kara; Satoru Katsuda; Yoshiaki Kanemaru; Richard Kelley; Caroline Kilbourne; Shunji Kitamoto; Shogo Kobayashi; Takayoshi Kohmura; Aya Kubota; Maurice Leutenegger; Michael Loewenstein; Yoshitomo Maeda; Maxim Markevitch; Hironori Matsumoto; Kyoko Matsushita; Dan McCammon; Brian McNamara; François Mernier; Eric D Miller; Jon M Miller; Ikuyuki Mitsuishi; Misaki Mizumoto; Tsunefumi Mizuno; Koji Mori; Koji Mukai; Hiroshi Murakami; Richard Mushotzky; Hiroshi Nakajima; Kazuhiro Nakazawa; Jan-Uwe Ness; Kumiko Nobukawa; Masayoshi Nobukawa; Hirofumi Noda; Hirokazu Odaka; Shoji Ogawa; Anna Ogorzalek; Takashi Okajima; Naomi Ota; Stephane Paltani; Robert Petre; Paul Plucinsky; Frederick Scott Porter; Katja Pottschmidt; Kosuke Sato; Toshiki Sato; Makoto Sawada; Hiromi Seta; Megumi Shidatsu; Aurora Simionescu; Randall Smith; Hiromasa Suzuki; Andrew Szymkowiak; Hiromitsu Takahashi; Mai Takeo; Toru Tamagawa; Keisuke Tamura; Takaaki Tanaka; Atsushi Tanimoto; Makoto Tashiro; Yukikatsu Terada; Yuichi Terashima; Yohko Tsuboi; Masahiro Tsujimoto; Hiroshi Tsunemi; Takeshi G Tsuru; Hiroyuki Uchida; Nagomi Uchida; Yuusuke Uchida; Hideki Uchiyama; Yoshihiro Ueda; Shinichiro Uno; Jacco Vink; Shin Watanabe; Brian J Williams; Satoshi Yamada; Shinya Yamada; Hiroya Yamaguchi; Kazutaka Yamaoka; Noriko Yamasaki; Makoto Yamauchi; Shigeo Yamauchi; Tahir Yaqoob; Tomokage Yoneyama; Tessei Yoshida; Mihoko Yukita; Irina Zhuravleva; Manan Agarwal; Yuken Ohshiro
  Publications of the Astronomical Society of Japan, Volume：76, Number：6, First page：1186, Last page：1201, Oct. 2024, [Reviewed]
  Abstract
  
  We present an initial analysis of the X-Ray Imaging and Spectroscopy Mission (XRISM) first-light observation of the supernova remnant (SNR) N 132D in the Large Magellanic Cloud. The Resolve microcalorimeter has obtained the first high-resolution spectrum in the 1.6–10 keV band, which contains K-shell emission lines of Si, S, Ar, Ca, and Fe. We find that the Si and S lines are relatively narrow, with a broadening represented by a Gaussian-like velocity dispersion of $\sigma _v \sim 450$ km s$^{-1}$. However, the Fe He$\alpha$ lines are substantially broadened with $\sigma _v \sim 1670$ km s$^{-1}$. This broadening can be explained by a combination of the thermal Doppler effect due to the high ion temperature and the kinematic Doppler effect due to the SNR expansion. Assuming that the Fe He$\alpha$ emission originates predominantly from the supernova ejecta, we estimate the reverse shock velocity at the time when the bulk of the Fe ejecta were shock heated to be $-1000 \lesssim V_{\rm rs}$ (km s$^{-1}$) $\lesssim 3300$ (in the observer frame). We also find that Fe Ly$\alpha$ emission is redshifted with a bulk velocity of $\sim 890$ km s$^{-1}$, substantially larger than the radial velocity of the local interstellar medium surrounding N 132D. These results demonstrate that high-resolution X-ray spectroscopy is capable of providing constraints on the evolutionary stage, geometry, and velocity distribution of SNRs.
  Oxford University Press (OUP), Scientific journal
  DOI：https://doi.org/10.1093/pasj/psae080
  DOI ID：10.1093/pasj/psae080, ISSN：0004-6264, eISSN：2053-051X
• XRISM Spectroscopy of the Fe Kα Emission Line in the Seyfert Active Galactic Nucleus NGC 4151 Reveals the Disk, Broad-line Region, and Torus　　　　　　　　　　　　　　　
  Marc Audard; Hisamitsu Awaki; Ralf Ballhausen; Aya Bamba; Ehud Behar; Rozenn Boissay-Malaquin; Laura Brenneman; Gregory V. Brown; Lia Corrales; Elisa Costantini; Renata Cumbee; Maria Diaz Trigo; Chris Done; Tadayasu Dotani; Ken Ebisawa; Megan E. Eckart; Dominique Eckert; Teruaki Enoto; Satoshi Eguchi; Yuichiro Ezoe; Adam Foster; Ryuichi Fujimoto; Yutaka Fujita; Yasushi Fukazawa; Kotaro Fukushima; Akihiro Furuzawa; Luigi Gallo; Javier A. García; Liyi Gu; Matteo Guainazzi; Kouichi Hagino; Kenji Hamaguchi; Isamu Hatsukade; Katsuhiro Hayashi; Takayuki Hayashi; Natalie Hell; Edmund Hodges-Kluck; Ann Hornschemeier; Yuto Ichinohe; Manabu Ishida; Kumi Ishikawa; Yoshitaka Ishisaki; Jelle Kaastra; Timothy Kallman; Erin Kara; Satoru Katsuda; Yoshiaki Kanemaru; Richard Kelley; Caroline Kilbourne; Shunji Kitamoto; Shogo Kobayashi; Takayoshi Kohmura; Aya Kubota; Maurice Leutenegger; Michael Loewenstein; Yoshitomo Maeda; Maxim Markevitch; Hironori Matsumoto; Kyoko Matsushita; Dan McCammon; Brian McNamara; François Mernier; Eric D. Miller; Jon M. Miller; Ikuyuki Mitsuishi; Misaki Mizumoto; Tsunefumi Mizuno; Koji Mori; Koji Mukai; Hiroshi Murakami; Richard Mushotzky; Hiroshi Nakajima; Kazuhiro Nakazawa; Jan Uwe Ness; Kumiko Nobukawa; Masayoshi Nobukawa; Hirofumi Noda; Hirokazu Odaka; Shoji Ogawa; Anna Ogorzalek; Takashi Okajima; Naomi Ota; Stephane Paltani; Robert Petre; Paul Plucinsky; Frederick S. Porter; Katja Pottschmidt; Kosuke Sato; Toshiki Sato; Makoto Sawada; Hiromi Seta; Megumi Shidatsu; Aurora Simionescu; Randall Smith; Hiromasa Suzuki; Andrew Szymkowiak; Hiromitsu Takahashi; Mai Takeo; Toru Tamagawa; Keisuke Tamura
  Astrophysical Journal Letters, Volume：973, Number：1, Sep. 2024, [Reviewed]
  We present an analysis of the first two XRISM/Resolve spectra of the well-known Seyfert-1.5 active galactic nucleus (AGN) in NGC 4151, obtained in 2023 December. Our work focuses on the nature of the narrow Fe Kα emission line at 6.4 keV, the strongest and most common X-ray line observed in AGN. The total line is found to consist of three components. Even the narrowest component of the line is resolved with evident Fe Kα,1 (6.404 keV) and Kα,2 (6.391 keV) contributions in a 2:1 flux ratio, fully consistent with neutral gas with negligible bulk velocity. Subject to the limitations of our models, the narrowest and intermediate-width components are consistent with emission from optically thin gas, suggesting that they arise in a disk atmosphere and/or wind. Modeling the three line components in terms of Keplerian broadening, they are readily associated with (1) the inner wall of the “torus,” (2) the innermost optical “broad-line region” (or “X-ray BLR”), and (3) a region with a radius of r; 100 GM/c2 that may signal a warp in the accretion disk. Viable alternative explanations of the broadest component include a fast-wind component and/or scattering; however, we find evidence of variability in the narrow Fe Kα line complex on timescales consistent with small radii. The best-fit models are statistically superior to simple Voigt functions, but when fit with Voigt profiles the time-averaged lines are consistent with a projected velocity broadening of FWHM = 1600-+200400 km s-1. Overall, the resolution and sensitivity of XRISM show that the narrow Fe K line in AGN is an effective probe of all key parts of the accretion flow, as it is currently understood. We discuss the implications of these findings for our understanding of AGN accretion, future studies with XRISM, and X-ray-based black hole mass measurements.
  Scientific journal
  DOI：https://doi.org/10.3847/2041-8213/ad7397
  Scopus：https://www.scopus.com/inward/record.uri?partnerID=HzOxMe3b&scp=85205840496&origin=inward
  Scopus Citedby：https://www.scopus.com/inward/citedby.uri?partnerID=HzOxMe3b&scp=85205840496&origin=inward
  DOI ID：10.3847/2041-8213/ad7397, ISSN：2041-8205, eISSN：2041-8213, SCOPUS ID：85205840496
• Evaluation of the initial pointing accuracy of XRISM　　　　　　　　　　　　　　　
  Yoshiaki Kanemaru; Ryo Iizuka; Yoshitomo Maeda; Takashi Okajima; Takayuki Hayashi; Kazuhiro Kiyokane; Yuto Nihei; Takashi Kominato; Manabu Ishida; Chikara Natsukari; Shin Watanabe; Kosuke Sato; Yukikatsu Terada; Katsuhiro Hayashi; Chris Baluta; Tessei Yoshida; Akio Hoshino; Shoji Ogawa; Kotaro Fukushima; Hiromitsu Takahashi; Masayoshi Nobukawa; Tsunefumi Mizuno; Kazuhiro Nakazawa; Shin'ichiro Uno; Ken Ebisawa; Satoshi Eguchi; Satoru Katsuda; Aya Kubota; Naomi Ota; Megumi Shidatsu; Atsushi Tanimoto; Yuichi Terashima; Yohko Tsuboi; Yuusuke Uchida; Hideki Uchiyama; Shigeo Yamauchi; Yoneyama Tomokage; Satoshi Yamada; Nagomi Uchida; Rie Sato; Matt Holland; Michael Loewenstein; Eric D. Miller; Tahir Yaqoob; Robert S. Hill; Trisha F. Doyle; Efrain Perez-Solis; Morgan D. Waddy; Mark Mekosh; Joseph B. Fox; Makoto S. Tashiro; Kenichi Toda; Hironori Maejima
  Space Telescopes and Instrumentation 2024: Ultraviolet to Gamma Ray, First page：224, Last page：224, Aug. 2024
  SPIE, International conference proceedings
  DOI：https://doi.org/10.1117/12.3016594
  DOI ID：10.1117/12.3016594
• Verification of the XRISM timing system in the GPS unsynchronized mode　　　　　　　　　　　　　　　
  Megumi Shidatsu; Yukikatsu Terada; Takashi Kominato; So Kato; Ryohei Sato; Minami Sakama; Takumi Shioiri; Yugo Motogami; Yuki Niida; Toshihiro Takagi; Chikara Natsukari; Makoto S. Tashiro; Kenichi Toda; Hironori Maejima; Shin Watanabe; Ryo Iizuka; Rie Sato; Chris Baluta; Katsuhiro Hayashi; Tessei Yoshida; Shoji Ogawa; Yoshiaki Kanemaru; Kotaro Fukushima; Akio Hoshino; Hiromitsu Takahashi; Masayoshi Nobukawa; Tsunefumi Mizuno; Kazuhiro Nakazawa; Shin'ichiro Uno; Ken Ebisawa; Satoshi Eguchi; Satoru Katsuda; Aya Kubota; Naomi Ota; Atsushi Tanimoto; Yuichi Terashima; Yohko Tsuboi; Yuusuke Uchida; Hideki Uchiyama; Shigeo Yamauchi; Tomokage Yoneyama; Satoshi Yamada; Nagomi Uchida; Matt Holland; Michael Loewenstein; Eric D. Miller; Tahir Yaqoob; Robert S. Hill; Trisha F. Doyle; Efrain Perez-Solis; Morgan D. Waddy; Mark Mekosh; Joseph B. Fox
  Space Telescopes and Instrumentation 2024: Ultraviolet to Gamma Ray, First page：235, Last page：235, Aug. 2024
  SPIE, International conference proceedings
  DOI：https://doi.org/10.1117/12.3019651
  DOI ID：10.1117/12.3019651
• Detail design of the XRISM Timing System and its verification in the nominal operation mode　　　　　　　　　　　　　　　
  Yukikatsu Terada; Megumi Shidatsu; Makoto Sawada; Takashi Kominato; So Kato; Ryohei Sato; Minami Sakama; Takumi Shioiri; Yuki Niida; Chikara Natsukari; Makoto S. Tashiro; Kenichi Toda; Hironori Maejima; Katsuhiro Hayashi; Tessei Yoshida; Shoji Ogawa; Yoshiaki Kanemaru; Akio Hoshino; Kotaro Fukushima; Hiromitsu Takahashi; Masayoshi Nobukawa; Tsunefumi Mizuno; Kazuhiro Nakazawa; Shin'ichiro Uno; Ken Ebisawa; Satoshi Eguchi; Satoru Katsuda; Aya Kubota; Naomi Ota; Atsushi Tanimoto; Yuichi Terashima; Yohko Tsuboi; Yuusuke Uchida; Hideki Uchiyama; Shigeo Yamauchi; Tomokage Yoneyama; Satoshi Yamada; Nagomi Uchida; Shin Watanabe; Ryo Iizuka; Rie Sato; Chris Baluta; Matt Holland; Michael Loewenstein; Eric D. Miller; Tahir Yaqoob; Robert S. Hill; Trisha F. Doyle; Efrain Perez-Solis; Morgan D. Waddy; Mark Mekosh; Joseph B. Fox; Toshihiro Takagi; Yugo Motogami; Katja Pottschmidt; Teruaki Enoto; Takaaki Tanaka
  Space Telescopes and Instrumentation 2024: Ultraviolet to Gamma Ray, First page：61, Last page：61, Aug. 2024
  SPIE, International conference proceedings
  DOI：https://doi.org/10.1117/12.3019329
  DOI ID：10.1117/12.3019329
• The in-orbit XRISM science operations　　　　　　　　　　　　　　　
  Katsuhiro Hayashi; Makoto S. Tashiro; Yukikatsu Terada; Tessei Yoshida; Shoji Ogawa; Yoshiaki Kanemaru; Kotaro Fukushima; Akio Hoshino; Hiromitsu Takahashi; Masayoshi Nobukawa; Tsunefumi Mizuno; Kazuhiro Nakazawa; Shin'ichiro Uno; Ken Ebisawa; Satoshi Eguchi; Satoru Katsuda; Takao Kitaguchi; Aya Kubota; Naomi Ota; Megumi Shidatsu; Atsushi Tanimoto; Yuichi Terashima; Yohko Tsuboi; Yuusuke Uchida; Hideki Uchiyama; Shigeo Yamauchi; Tomokage Yoneyama; Satoshi Yamada; Nagomi Uchida; Seiko Sakurai; Shin Watanabe; Ryo Iizuka; Rie Sato; Chris Baluta; Takayuki Tamura; Yasushi Fukazawa; Hirokazu Odaka; Tsubasa Tamba; Ryohei Sato; Sou Kato; Minami Sakama; Takumi Shioiri; Yuki Niida; Natsuki Sakamoto; Noboru Nemoto; Yuki Omiya; Nari Suzuki; Toshihiro Takagi; Yugo Motogami; Matt Holland; Michael Loewenstein; Eric D. Miller; Tahir Yaqoob; Robert S. Hill; Trisha F. Doyle; Efrain Perez-Solis; Morgan D. Waddy; Mark Mekosh; Joseph B. Fox; Matteo Guainazzi; Jan-Uwe Ness; Hironori Maejima; Kenichi Toda; Chikara Natsukari
  Space Telescopes and Instrumentation 2024: Ultraviolet to Gamma Ray, First page：60, Last page：60, Aug. 2024
  SPIE, International conference proceedings
  DOI：https://doi.org/10.1117/12.3018908
  DOI ID：10.1117/12.3018908
• Development and operation status of X-Ray Imaging and Spectroscopy Mission (XRISM)　　　　　　　　　　　　　　　
  Makoto S. Tashiro; Shin Watanabe; Hironori Maejima; Kenichi Toda; Kyoko Matsushita; Hiroya Yamaguchi; Richard L. Kelley; Lillian S. Reichenthal; Leslie S. Hartz; Robert Petre; Brian J. Williams; Matteo Guainazzi; Andrea Santovincenzo; Elisa Costantini; Yoh Takei; Yoshitaka Ishisaki; Ryuichi Fujimoto; Joy Henegar-Leon; Gary Sneiderman; Hiroshi Tomida; Koji Mori; Hiroshi Nakajima; Yukikatsu Terada; Matt Holland; Micheal Loewenstein; Tomothey Kallman; Jelle Kaastra; Eric Miller; Makoto Sawada; Chris Done; Teruaki Enoto; Aya Bamba; Paul Plucinsky; Yoshitaka Ueda; Erin Kara; Irina Zhuravleva; Yutaka Fujita; Jose Antonio Quero; Yoshitaka Arai; Marc Audard; Hisamitsu Awaki; Chris Baluta; Nobutaka Bando; Ehud Behar; Thomas Bialas; Rozenn Boissay-Malaquin; Laura Brenneman; Gregory V. Brown; Meng Chiao; Lia Corrales; Renata Cumbee; Cor de Vries; Jan-Willem den Herder; Maria Diaz-Trigo; Michael DiPirro; Tadayasu Dotani; Jacobo Ebrero Carrero; Ken Ebisawa; Megan Eckart; Dominique Eckart; Satoshi Eguchi; Yuichiro Ezoe; Carlo Ferrgno; Adam Foster; Yasushi Fukazawa; Kotaro Fukushima; Akihiro Furuzawa; Luigi Gallo; Nathalie Gorter; Martin Grim; Liyi Gu; Koichi Hagino; Kenji Hamaguchi; Isamu Hatsukade; Katsuhiro Hayashi; Takayuki Hayashi; Natalie Hell; Edmund Hodges-Kluck; Takafumi Horiuchi; Ann Hornschemeier; Akio Hoshino; Yuto Ichinohe; Chisato Ikuta; Ryo Iizuka; Daiki Ishi; Manabu Ishida; Naoki Ishihama; Kumi Ishikawa; Kosei Ishimura; Tess Jaffe; Satoru Katsuda; Yoshiaki Kanemaru; Steven Kenyon; Caroline Kilbourne; Mark Kimball; Shunji Kitamoto; Shogo Kobayashi; Akihide Kobayashi; Takayoshi Kohmura; Aya Kubota; Maurice Leutenegger; Muzi Li; Yoshitomo Maeda; Maxim Markevitch; Hironori Matsumoto; Keiichi Matsuzaki; Dan McCammon; Brian McLaughlin; Brian McNamara; Josegh Miko; Jon Miller; Kenji Minesugi; Shinji Mitani; Ikuyuki Mitsuishi; Misaki Mizumoto; Tsunefumi Mizuno; Koji Mukai; Hiroshi Murakami; Richard Mushotzky; Kazuhiro Nakazawa; Chikara Natsukari; Jan-Uwe Ness; Kenichiro Nigo; Mari Nishiyama; Kumiko Nobukawa; Masayoshi Nobukawa; Hirofumi Noda; Hirokazu Odaka; Mina Ogawa; Shoji Ogawa; Takashi Okajima; Atsushi Okamoto; Naomi Ota; Masanobu Ozaki; Stephane Paltani; F. Scott Porter; Katja Pottschmidt; Takahiro Sasaki; Kosuke Sato; Rie Sato; Toshiki Sato; Yoichi Sato; Hiromi Seta; Maki Shida; Megumi Shidatsu; Shuhei Shigeto; Russel Shipman; Keisuke Shinozaki; Peter Shirron; Aurora Simionescu; Randall Smith; Young Soong; Hiromasa Suzuki; Andy Szymkowiak; Hiromitsu Takahashi; Mai Takeo; Toru Tamagawa; Keisuke Tamura; Takaaki Tanaka; Atsushi Tanimoto; Yoichi Terashima; Yohko Tsuboi; Masahiro Tsujimoto; Hiroshi Tsunemi; Takeshi Tsuru; Hiroyuki Uchida; Nagomi Ucghida; Yuusuke Uchida; Hideki Uchiyama; Shinichiro Uno; Erik Van der Meer; Jacco Vink; Michael Wittheof; Rob Wolf; Satoshi Yamada; Shinya Yamada; Kazutaka Yamaoka; Noriko Yamasaki; Makoto Yamauchi; Shigeo Yamauchi; Keiichi Yamagase; Tahir Yaqoob; Susumu Yasuda; Tomokage Yoneyama; Tessei Yoshida
  Space Telescopes and Instrumentation 2024: Ultraviolet to Gamma Ray, First page：52, Last page：52, Aug. 2024, [Lead, Corresponding]
  SPIE, International conference proceedings
  DOI：https://doi.org/10.1117/12.3019325
  DOI ID：10.1117/12.3019325
• ALMA ACA Detection of Submillimeter Emission Associated with the Western Hot Spot of the Radio Galaxy Pictor A　　　　　　　　　　　　　　　
  Naoki Isobe; Hiroshi Nagai; Motoki Kino; Shunsuke Baba; Takao Nakagawa; Yuji Sunada; Makoto Tashiro
  The Astrophysical Journal, Aug. 2023, [Reviewed]
  Scientific journal
  DOI：https://doi.org/10.3847/1538-4357/ace04d
  DOI ID：10.3847/1538-4357/ace04d, ORCID：139815978
• Long‐Term Density Trend in the Mesosphere and Lower Thermosphere From Occultations of the Crab Nebula With X‐Ray Astronomy Satellites
  Satoru Katsuda; Teruaki Enoto; Andrea N. Lommen; Koji Mori; Yuko Motizuki; Motoki Nakajima; Nathaniel C. Ruhl; Kosuke Sato; Gunter Stober; Makoto S. Tashiro; Yukikatsu Terada; Kent S. Wood
  Journal of Geophysical Research: Space Physics, Volume：128, Number：2, Feb. 2023, [Reviewed]
  American Geophysical Union (AGU), English, Scientific journal
  DOI：https://doi.org/10.1029/2022JA030797
  DOI ID：10.1029/2022JA030797, ISSN：2169-9380, eISSN：2169-9402, ORCID：127812939
• Frontiers in accretion physics at high X-ray spectral resolution
  P. Gandhi; T. Kawamuro; M. Díaz Trigo; J. A. Paice; P. G. Boorman; M. Cappi; C. Done; A. C. Fabian; K. Fukumura; J. A. García; C. L. Greenwell; M. Guainazzi; K. Makishima; M. S. Tashiro; R. Tomaru; F. Tombesi; Y. Ueda
  Nature Astronomy, Volume：6, Number：12, First page：1364, Last page：1375, Dec. 2022, [Reviewed]
  Springer Science and Business Media LLC, English, Scientific journal
  DOI：https://doi.org/10.1038/s41550-022-01857-y
  DOI ID：10.1038/s41550-022-01857-y, eISSN：2397-3366
• Simultaneous radio and optical polarimetry of GRB 191221B afterglow
  Yuji Urata; Kenji Toma; Stefano Covino; Klaas Wiersema; Kuiyun Huang; Jiro Shimoda; Asuka Kuwata; Sota Nagao; Keiichi Asada; Hiroshi Nagai; Satoko Takahashi; Chao-En Chung; Glen Petitpas; Kazutaka Yamaoka; Luca Izzo; Johan Fynbo; Antonio de Ugarte Postigo; Maryam Arabsalmani; Makoto Tashiro
  Nature Astronomy, Volume：7, Number：1, First page：80, Last page：87, Dec. 2022, [Reviewed]
  Springer Science and Business Media LLC, Scientific journal
  DOI：https://doi.org/10.1038/s41550-022-01832-7
  DOI ID：10.1038/s41550-022-01832-7, eISSN：2397-3366
• Vibration Characteristics of a Continuously Rotating Superconducting Magnetic Bearing and Potential Influence to TES and SQUID
  S. Sugiyama; T. Ghigna; Y. Hoshino; N. Katayama; S. Katsuda; K. Komatsu; T. Matsumura; Y. Sakurai; K. Sato; R. Takaku; M. Tashiro; Y. Terada
  Journal of Low Temperature Physics, Volume：209, Number：5-6, First page：1088, Last page：1096, Sep. 2022, [Reviewed]
  Springer Science and Business Media LLC, English, Scientific journal
  DOI：https://doi.org/10.1007/s10909-022-02846-1
  DOI ID：10.1007/s10909-022-02846-1, ISSN：0022-2291, eISSN：1573-7357
• Xappl: software framework for the XRISM pre-pipeline　　　　　　　　　　　　　　　
  Satoshi Eguchi; Makoto Tashiro; Yukikatsu Terada; Hiromitsu Takahashi; Masayoshi Nobukawa; Tsunefumi Mizuno; Shin'ichiro Uno; Aya Kubota; Kazuhiro Nakazawa; Shin Watanabe; Ryo Iizuka; Rie Sato; Tomokage Yoneyama; Chris Baluta; Ken Ebisawa; Yasushi Fukazawa; Katsuhiro Hayashi; So Kato; Satoru Katsuda; Takao Kitaguchi; Hirokazu Odaka; Masanori Ohno; Naomi Ota; Minami Sakama; Ryohei Sato; Megumi Shidatsu; Yasuharu Sugawara; Tsubasa Tamba; Atsushi Tanimoto; Yuichi Terashima; Yohko Tsuboi; Nagomi Uchida; Yuusuke Uchida; Hideki Uchiyama; Shigeo Yamauchi; Masaaki Sakano; Tessei Yoshida; Satoshi Yamada
  Space Telescopes and Instrumentation 2022: Ultraviolet to Gamma Ray, Aug. 2022, [Reviewed]
  SPIE, International conference proceedings
  DOI：https://doi.org/10.1117/12.2629316
  DOI ID：10.1117/12.2629316
• NuSTAR discovery of the hard X-ray emission and a wide-band X-ray spectrum from the Pictor A western hotspot　　　　　　　　　　　　　　　
  Yuji Sunada; Arisa Morimoto; Makoto S Tashiro; Yukikatsu Terada; Satoru Katsuda; Kosuke Sato; Dai Tateishi; Nobuaki Sasaki
  Publications of the Astronomical Society of Japan, Jun. 2022, [Reviewed]
  English, Scientific journal
  DOI：https://doi.org/10.1093/pasj/psac022
  DOI ID：10.1093/pasj/psac022, ORCID：112971659
• Herschel discovery of far-infrared emission from the hotspot D in the radio galaxy Cygnus A
  Yuji Sunada; Naoki Isobe; Makoto S Tashiro; Motoki Kino; Shoko Koyama; Satomi Nakahara
  Monthly Notices of the Royal Astronomical Society, Volume：512, Number：4, First page：5995, Last page：6006, Apr. 2022, [Reviewed]
  Abstract
  
  The far infrared counterpart of hot spot D, the terminal hot spot of the eastern jet hosted by the radio galaxy Cygnus A, is detected with Herschel Aperture photometery of the source performed in 5 photometric bands covering the wavelength range of 70–350 μm. After removing the contamination from another nearby hot spot, E, the far-infrared intensity of hot spot D is derived as 83 ± 13 and 269 ± 66 mJy at 160 and 350 μm, respectively. Since the far-infrared spectrum of the object smoothly connects to the radio one, the far-infrared emission is attributed to the synchrotron radiation from the radio-emitting electron population. The radio-to-near-infrared spectrum is confirmed to exhibit a far-infrared break feature at the frequency of $\nu _\mathrm{br}=2.0^{+1.2}_{-0.8} \times 10^{12}$ Hz. The change in energy index at the break (Δα = 0.5) is interpreted as the impact of radiative cooling on an electron distribution sustained by continuous injection from diffusive shock acceleration. By ascribing the derived break to this cooling break, the magnetic field, B, in the hot spot is determined as a function of its radius, R within a uniform one-zone model combined with the strong relativistic shock condition. An independent B-R constraint is obtained by assuming the X-ray spectrum is wholly due to synchrotron-self-Compton emission. By combining these conditions, the two parameters are tightly determined as B = 120–150 μG and R = 1.3–1.6 kpc. A further investigation into the two conditions indicates the observed X-ray flux is highly dominated by the synchrotron-self-Compton emission.
  Oxford University Press (OUP), English, Scientific journal
  DOI：https://doi.org/10.1093/mnras/stac826
  DOI ID：10.1093/mnras/stac826, ISSN：0035-8711, eISSN：1365-2966, ORCID：111636947
• XRISM: X-ray imaging and spectroscopy mission　　　　　　　　　　　　　　　
  Tashiro; Makoto S
  International Journal of Modern Physics D,, Volume：31, Number：2, First page：id 2230001, Jan. 2022, [Reviewed], [Invited], [Lead]
  English, International conference proceedings
  DOI：https://doi.org/10.1142/S0218271822300014
  DOI ID：10.1142/S0218271822300014
• Detailed design of the science operations for the XRISM mission　　　　　　　　　　　　　　　
  Yukikatsu Terada; Matt Holland; Michael Loewenstein; Makoto Tashiro; Hiromitsu Takahashi; Masayoshi Nobukawa; Tsunefumi Mizuno; Takayuki Tamura; Shin’ichiro Uno; Shin Watanabe; Chris Baluta; Laura Burns; Ken Ebisawa; Satoshi Eguchi; Yasushi Fukazawa; Katsuhiro Hayashi; Ryo Iizuka; Satoru Katsuda; Takao Kitaguchi; Aya Kubota; Eric Miller; Koji Mukai; Shinya Nakashima; Kazuhiro Nakazawa; Hirokazu Odaka; Masanori Ohno; Naomi Ota; Rie Sato; Makoto Sawada; Yasuharu Sugawara; Megumi Shidatsu; Tsubasa Tamba; Atsushi Tanimoto; Yuichi Terashima; Yohko Tsuboi; Yuusuke Uchida; Hideki Uchiyama; Shigeo Yamauchi; Tahir Yaqoob
  Journal of Astronomical Telescopes, Instruments, and Systems, Volume：7, Number：03, Jul. 2021, [Reviewed]
  SPIE-Intl Soc Optical Eng, Scientific journal
  DOI：https://doi.org/10.1117/1.jatis.7.3.037001
  DOI ID：10.1117/1.jatis.7.3.037001, ISSN：2329-4124
• Planning in-flight calibration for XRISM　　　　　　　　　　　　　　　
  Eric D. Miller; Makoto Sawada; Matteo Guainazzi; Aurora Simionescu; Maxim Markevitch; Liyi Gu; Megan E. Eckart; Caroline A. Kilbourne; Maurice A. Leutenegger; Frederick S. Porter; Masahiro Tsujimoto; Cor P. de Vries; Takashi Okajima; Takayuki Hayashi; Rozenn Boissay-Malaquin; Keisuke Tamura; Hironori Matsumoto; Koji Mori; Hiroshi Nakajima; Takaaki Tanaka; Yukikatsu Terada; Michael Loewenstein; Tahir Yaqoob; Marc Audard; Ehud Behar; Laura Brenneman; Lia Corrales; Renata S. Cumbee; Teruaki Enoto; Edmund Hodges-Kluck; Yoshitomo Maeda; Paul P. Plucinsky; Katja Pottschmidt; Makoto S. Tashiro; Richard L. Kelley; Robert Petre; Brian J. Williams; Hiroya Yamaguchi
  Space Telescopes and Instrumentation 2020: Ultraviolet to Gamma Ray, Dec. 2020
  SPIE, International conference proceedings
  DOI：https://doi.org/10.1117/12.2561608
  DOI ID：10.1117/12.2561608
• Status of x-ray imaging and spectroscopy mission (XRISM)　　　　　　　　　　　　　　　
  Makoto S. Tashiro; Hironori Maejima; Kenichi Toda; Richard L. Kelley; Lillian Reichenthal; Leslie Hartz; Robert Petre; Brian J. Williams; Matteo Guainazzi; Elisa Costantini; Ryuichi Fujimoto; Kiyoshi Hayashida; Joy Henegar-Leon; Matt Holland; Yoshitaka Ishisaki; Caroline Kilbourne; Mike Loewenstein; Kyoko Matsushita; Koji Mori; Takashi Okajima; F. Scott Porter; Gary Sneiderman; Yoh Takei; Yukikatsu Terada; Hiroshi Tomida; Hiroya Yamaguchi; Shin Watanabe; Hiroki Akamatsu; Yoshitaka Arai; Marc Audard; Hisamitsu Awaki; Iurii Babyk; Aya Bamba; Nobutaka Bando; Ehud Behar; Thomas Bialas; Rozenn Boissay-Malaquin; Laura Brenneman; Greg Brown; Edgar Canavan; Meng Chiao; Brian Comber; Lia Corrales; Renata Cumbee; Cor de Vries; Jan-Willem den Herder; Johannes Dercksen; Maria Diaz-Trigo; Michael DiPirro; Chris Done; Tadayasu Dotani; Ken Ebisawa; Megan Eckart; Dominique Eckert; Satoshi Eguchi; Teruaki Enoto; Yuichiro Ezoe; Carlo Ferrigno; Yutaka Fujita; Yasushi Fukazawa; Akihiro Furuzawa; Luigi Gallo; Nathalie Gorter; Martin Grim; Liyi Gu; Kouichi Hagino; Kenji Hamaguchi; Isamu Hatsukade; David Hawthorn; Katsuhiro Hayashi; Natalie Hell; Junko Hiraga; Edmund Hodges-Kluck; Takafumi Horiuchi; Ann Hornschemeier; Akio Hoshino; Yuto Ichinohe; Sayuri Iga; Ryo Iizuka; Manabu Ishida; Naoki Ishihama; Kumi Ishikawa; Kosei Ishimura; Tess Jaffe; Jelle Kaastra; Timothy Kallman; Erin Kara; Satoru Katsuda; Steven Kenyon; Mark Kimball; Takao Kitaguti; Shunji Kitamoto; Shogo Kobayashi; Akihide Kobayashi; Takayoshi Kohmura; Aya Kubota; Maurice Leutenegger; Muzi Li; Tom Lockard; Yoshitomo Maeda; Maxim Markevitch; Connor Martz; Hironori Matsumoto; Keiichi Matsuzaki; Dan McCammon; Brian McLaughlin; Brian McNamara; Joseph Miko; Eric Miller; Jon Miller; Kenji Minesugi; Shinji Mitani; Ikuyuki Mitsuishi; Misaki Mizumoto; Tsunefumi Mizuno; Koji Mukai; Hiroshi Murakami; Richard Mushotzky; Hiroshi Nakajima; Hideto Nakamura; Kazuhiro Nakazawa; Chikara Natsukari; Kenichiro Nigo; Yusuke Nishioka; Kumiko Nobukawa; Masayoshi Nobukawa; Hirofumi Noda; Hirokazu Odaka; Mina Ogawa; Takaya Ohashi; Masahiro Ohno; Masayuki Ohta; Atsushi Okamoto; Naomi Ota; Masanobu Ozaki; Stephane Paltani; Paul Plucinsky; Katja Pottschmidt; Michael Sampson; Takahiro Sasaki; Kosuke Sato; Rie Sato; Toshiki Sato; Makoto Sawada; Hiromi Seta; Yasuko Shibano; Maki Shida; Megumi Shidatsu; Shuhei Shigeto; Keisuke Shinozaki; Peter Shirron; Aurora Simionescu; Randall Smith; Kazunori Someya; Yang Soong; Keisuke Sugawara; Yasuharu Sugawara; Andy Szymkowiak; Hiromitsu Takahashi; Toshiaki Takeshima; Toru Tamagawa; Keisuke Tamura; Takaaki Tanaka; Atsushi Tanimoto; Yuichi Terashima; Yohko Tsuboi; Masahiro Tsujimoto; Hiroshi Tsunemi; Takeshi Tsuru; Hiroyuki Uchida; Yuusuke Uchida; Hideki Uchiyama; Yoshihiro Ueda; Shinichiro Uno; Jacco Vink; Tomomi Watanabe; Michael Wittheof; Rob Wolfs; Shinya Yamada; Kazutaka Yamaoka; Noriko Yamasaki; Makoto Yamauchi; Shigeo Yamauchi; Keiichi Yanagase; Tahir Yaqoob; Susumu Yasuda; Tessei Yoshida; Nasa Yoshioka; Irina Zhuravleva
  Space Telescopes and Instrumentation 2020: Ultraviolet to Gamma Ray, Dec. 2020, [Lead, Corresponding]
  SPIE, International conference proceedings
  DOI：https://doi.org/10.1117/12.2565812
  DOI ID：10.1117/12.2565812
• New Measurement of the Vertical Atmospheric Density Profile from Occultations of the Crab Nebula with X-Ray Astronomy Satellites Suzaku and Hitomi
  Satoru Katsuda; Hitoshi Fujiwara; Yoshitaka Ishisaki; Yoshitomo Maeda; Koji Mori; Yuko Motizuki; Kosuke Sato; Makoto S Tashiro; Yukikatsu Terada
  Journal of Geophysical Research: Space Physics, Volume：126, Number：4, Nov. 2020, [Reviewed]
  Wiley, Scientific journal
  DOI：https://doi.org/10.1002/essoar.10504733.1
  DOI ID：10.1002/essoar.10504733.1, ISSN：2169-9380, eISSN：2169-9402, ORCID：84039593
• Herschel SPIRE Discovery of Far-infrared Excess Synchrotron Emission from the West Hot Spot of the Radio Galaxy Pictor A
  Naoki Isobe; Yuji Sunada; Motoki Kino; Shoko Koyama; Makoto Tashiro; Hiroshi Nagai; Chris Pearson
  The Astrophysical Journal, Volume：899, Number：1, First page：17, Last page：17, Aug. 2020, [Reviewed]
  American Astronomical Society, Scientific journal
  DOI：https://doi.org/10.3847/1538-4357/ab9d1c
  DOI ID：10.3847/1538-4357/ab9d1c, eISSN：1538-4357, ORCID：78445287
• Inverse First Ionization Potential Effects in Giant Solar Flares Found from Earth X-Ray Albedo with Suzaku/XIS
  Satoru Katsuda; Masanori Ohno; Koji Mori; Tatsuhiko Beppu; Yoshiaki Kanemaru; Makoto S. Tashiro; Yukikatsu Terada; Kosuke Sato; Kae Morita; Hikari Sagara; Futa Ogawa; Haruya Takahashi; Hiroshi Murakami; Masayoshi Nobukawa; Hiroshi Tsunemi; Kiyoshi Hayashida; Hironori Matsumoto; Hirofumi Noda; Hiroshi Nakajima; Yuichiro Ezoe; Yohko Tsuboi; Yoshitomo Maeda; Takaaki Yokoyama; Noriyuki Narukage
  The Astrophysical Journal, Volume：891, Number：2, First page：126, Last page：126, Mar. 2020, [Reviewed]
  American Astronomical Society, Scientific journal
  DOI：https://doi.org/10.3847/1538-4357/ab7207
  DOI ID：10.3847/1538-4357/ab7207, eISSN：1538-4357, ORCID：77236401
• Systematic Study of the Peak Energy of Broadband Gamma-Ray Burst Spectra　　　　　　　　　　　　　　　
  Daisuke Katsukura; Takanori Sakamoto; Makoto S. Tashiro; Yukikatsu Terada
  The Astrophysical Journal, Volume：889, Number：2, Feb. 2020
  We have performed a systematic study of gamma-ray bursts (GRBs), which have various values in the peak energy of the νF ν spectrum of prompt emission, E peak, observed by the Swift/Burst Alert Telescope (BAT) and Fermi/Gamma-ray Burst Monitor, investigating their prompt and X-ray afterglow emissions. We cataloged long-lasting GRBs observed by Swift between 2004 December and 2014 February in three categories according to the classification by Sakamoto et al.: X-ray flashes (XRFs), X-ray-rich GRBs (XRRs), and classical GRBs (C-GRBs). We then derived E peak-obs, as well as E peak-src if viable, of the Swift spectra of their prompt emission. We also analyzed their X-ray afterglows and found that GRB events with a lower E, i.e., softer GRBs, are fainter in 0.3-10 keV X-ray luminosity and decay more slowly than harder GRBs. The intrinsic event rates of the XRFs, XRRs, and C-GRBs were calculated using the Swift/BAT trigger algorithm. Those of the XRRs and XRFs are larger than that of the C-GRBs. If we assume that the observational diversity of E peak is explained using the off-axis model, these results yield a jet half-opening angle of Δθ ∼ 0.°3, and a variance of the observing angles θ obs ≲ 0.°6. This implies that this tiny variance would be responsible for the E peak diversity observed by Swift/BAT, which is unrealistic. Therefore, we conclude that the E peak diversity is not explained with the off-axis model, but is likely to originate from some intrinsic properties of the jets.
  Institute of Physics Publishing, English, Scientific journal
  DOI：https://doi.org/10.3847/1538-4357/ab6167
  DOI ID：10.3847/1538-4357/ab6167, ISSN：1538-4357, ORCID：127132505, SCOPUS ID：85081288978
• The Hot Universe with XRISM and Athena　　　　　　　　　　　　　　　
  M. Guainazzi; M. S. Tashiro
  Proceedings of the International Astronomical Union, First page：29, Last page：36, 2020
  X-ray spectroscopy is key to address the theme of "The Hot Universe", the still poorly understood astrophysical processes driving the cosmological evolution of the baryonic hot gas traceable through its electromagnetic radiation. Two future X-ray observatories: The JAXA-led XRISM (due to launch in the early 2020s), and the ESA Cosmic Vision L-class mission Athena (early 2030s) will provide breakthroughs in our understanding of how and when large-scale hot gas structures formed in the Universe, and in tracking their evolution from the formation epoch to the present day.
  Cambridge University Press, English, Scientific journal
  DOI：https://doi.org/10.1017/S1743921318007792
  DOI ID：10.1017/S1743921318007792, ISSN：1743-9221, SCOPUS ID：85083432802
• The XRISM science data center: Optimizing the scientific return from a unique X-ray observatory　　　　　　　　　　　　　　　
  Michael Loewenstein; Robert S. Hill; Matthew P. Holland; Eric D. Miller; Tahir Yaqoob; Trisha F. Doyle; Patricia L. Hall; Efrem Braun; Chris Baluta; Koji Mukai; Yukikatsu Terada; Makoto Tashiro; Hiromitsu Takahashi; Masayoshi Nobukawa; Tsunefumi Mizuno; Takayuki Tamura; Shin'ichiro Uno; Shin Watanabe; Ken Ebisawa; Satoshi Eguchi; Yasushi Fukazawa; Katsuhiro Hayashi; Ryo Iizuka; Satoru Katsuda; Takao Kitaguchi; Aya Kubota; Shinya Nakashima; Kazuhiro Nakazawa; Hirokazu Odaka; Masanori Ohno; Naomi Ota; Rie Sato; Yasuharu Sugawara; Megumi Shidatsu; Tsubasa Tamba; Atsushi Tanimoto; Yuichi Terashima; Yohko Tsuboi; Yuusuke Uchida; Hideki Uchiyama; Shigeo Yamauchiq
  Proceedings of SPIE - The International Society for Optical Engineering, Volume：11444, 2020
  © 2020 SPIE The X-Ray Imaging and Spectroscopy Mission, XRISM, is currently scheduled to launch in 2022 with the objective of building on the brief, but significant, successes of the ASTRO-H (Hitomi) mission in solving outstanding astrophysical questions using high resolution X-ray spectroscopy. The XRISM Science Operations Team (SOT) consists of the JAXA-led Science Operations Center (SOC) and NASA-led Science Data Center (SDC), which work together to optimize the scientific output from the Resolve high-resolution spectrometer and the Xtend wide-field imager through planning and scheduling of observations, processing and distribution of data, development and distribution of software tools and the calibration database (CaldB), support of ground and in-flight calibration, and support of XRISM users in their scientific investigations of the energetic universe. Here, we summarize the roles and responsibilities of the SDC and its current status and future plans. The Resolve instrument poses particular challenges due to its unprecedented combination of high spectral resolution and throughput, broad spectral coverage, and relatively small field-of-view and large pixel-size. We highlight those challenges and how they are being met.
  International conference proceedings
  DOI：https://doi.org/10.1117/12.2560840
  Scopus：https://www.scopus.com/inward/record.uri?partnerID=HzOxMe3b&scp=85099287387&origin=inward
  Scopus Citedby：https://www.scopus.com/inward/citedby.uri?partnerID=HzOxMe3b&scp=85099287387&origin=inward
  DOI ID：10.1117/12.2560840, ISSN：0277-786X, eISSN：1996-756X, SCOPUS ID：85099287387
• Detail plans and preparations for the science operations of the XRISM mission　　　　　　　　　　　　　　　
  Yukikatsu Terada; Matt Holland; Michael Loewenstein; Makoto Tashiro; Hiromitsu Takahashi; Masayoshi Nobukawa; Tsunefumi Mizuno; Takayuki Tamura; Shin'ichiro Uno; Shin Watanabe; Chris Baluta; Laura Burns; Ken Ebisawa; Satoshi Eguchi; Yasushi Fukazawa; Katsuhiro Hayashi; Ryo Iizuka; Satoru Katsuda; Takao Kitaguchi; Aya Kubota; Eric Miller; Koji Mukai; Shinya Nakashima; Kazuhiro Nakazawa; Hirokazu Odaka; Masanori Ohno; Naomi Ota; Rie Sato; Yasuharu Sugawara; Megumi Shidatsu; Tsubasa Tamba; Atsushi Tanimoto; Yuichi Terashima; Yohko Tsuboi; Yuusuke Uchida; Hideki Uchiyama; Shigeo Yamauchi; Tahir Yaqoob
  Proceedings of SPIE - The International Society for Optical Engineering, Volume：11444, 2020
  © 2020 SPIE The XRISM is the X-ray astronomical mission led by JAXA/NASA/ESA with international participation, plan to be launched in 2022 (Japanese fiscal year), to quickly recover the high-resolution X-ray spectroscopy of astrophysical objects using the micro-calorimeter array after the failure of Hitomi. To enhance the scientific outputs of the mission, the Science Operations Team (SOT) is structured independently from the instrument teams and the mission operation team (MOT). The responsibilities of the SOT are summarized into four categories: 1) Guest observer program and data distributions, 2) Distribution of the analyses software and calibration database, 3) Guest observer supporting activities, and 4) the performance verification and optimization (PVO) activities. Before constructing the Operations Concept of the XRISM mission, the lessons on the Science Operations learned from the past Japanese X-ray missions (ASCA, Suzaku, and Hitomi) are reviewed, and 16 kinds of lessons are identified by the above categories: lessons on the importance of avoiding nonpublic (“animal”) tools, coding quality of public tools both on the engineering viewpoint and the calibration accuracy, tight communications with instrument teams and operations team, well-defined task division between scientists and engineers etc. Among these lessons, a) importance of the early preparations of the operations from the ground stage, b) construction of the independent team for the Science Operations from the instrument developments, and c) operations with well-defined duties by appointed members are recognized as the key lessons for XRISM. Then, i) the task division between the Mission and Science Operations and ii) the subgroup structure within the XRISM team are defined in detail as the XRISM Operations Concept. Then, following the Operations Concept, the detail plan of the Science Operations is designed as follows. The Science Operations tasks are shared among Japan, US, and Europe operated by three centers, the Science Operations Center (SOC) at JAXA, the Science Data Center (SDC) at NASA, and European Space Astronomy Centre (ESAC) at ESA. The SOT is defined as a combination of the SOC and SDC; the SOC is designed to perform tasks close to the spacecraft operations, such as spacecraft planning of science targets, quick-look health checks, pre-pipeline data processing, etc., and the SDC covers the tasks on the data calibration processing (pipeline processing), maintenance of the analysis tools etc. The data-archive and users-support activities are planned to be covered both by the SOC and SDC. Finally, the details of the Science Operations tasks and the tools for the Science Operations are also described in this paper. This information would be helpful for a construction of Science Operations of future X-ray missions.
  International conference proceedings
  DOI：https://doi.org/10.1117/12.2560861
  Scopus：https://www.scopus.com/inward/record.uri?partnerID=HzOxMe3b&scp=85099288779&origin=inward
  Scopus Citedby：https://www.scopus.com/inward/citedby.uri?partnerID=HzOxMe3b&scp=85099288779&origin=inward
  DOI ID：10.1117/12.2560861, ISSN：0277-786X, eISSN：1996-756X, SCOPUS ID：85099288779
• First Detection of Radio Linear Polarization in a Gamma-Ray Burst Afterglow
  Yuji Urata; Kenji Toma; Kuiyun Huang; Keiichi Asada; Hiroshi Nagai; Satoko Takahashi; Glen Petitpas; Makoto Tashiro; Kazutaka Yamaoka
  The Astrophysical Journal, Volume：884, Number：2, First page：L58, Last page：L58, Oct. 2019, [Reviewed]
  American Astronomical Society, Scientific journal
  DOI：https://doi.org/10.3847/2041-8213/ab48f3
  DOI ID：10.3847/2041-8213/ab48f3, eISSN：2041-8213
• Spectral properties of gamma-ray bursts observed by the Suzaku wide-band all-sky monitor　　　　　　　　　　　　　　　
  Norisuke Ohmori; Kazutaka Yamaoka; Makoto Yamauchi; Yuji Urata; Masanori Ohno; Satoshi Sugita; Kevin Hurley; Makoto S. Tashiro; Yasushi Fukazawa; Wataru Iwakiri; Daisuke Katsukura; Motohide Kokubun; Kazuo Makishima; Souta Murakami; Yujin E. Nakagawa; Kazuhiro Nakazawa; Katsuya Odaka; Kaito Takahashi; Tadayuki Takahashi; Yukikatsu Terada
  Publications of the Astronomical Society of Japan, Volume：71, Number：4, Aug. 2019
  We have systematically studied the spectral properties of 302 localized gamma-ray bursts (GRBs) observed by the Suzaku wide-band all-sky monitor (WAM) from 2005 August to 2010 December. The energy spectra in the 100-5000 keV range integrated over the entire emission and the 1 s peak were fitted by three models: a single power law, a power law with an exponential cutoff (CPL), and the GRB Band function (GRB). Most of the burst spectra were well fitted by a single power law. The average photon index α was -2.11 and -1.73 for long and short bursts, respectively. For the CPL and GRB models, the low-energy and high-energy photon indices (α and β) for the entire emission spectra were consistent with previous measurements. The averages of the α and β were -0.90 and -2.65 for long-duration GRBs, while the average α was -0.55 and the β was not well constrained for short-duration GRBs. However, the average peak energy Epeak was 645 and 1286 keV for long- and short-duration GRBs respectively, which are higher than previous Fermi/GBM measurements (285 keV and 736 keV). The α and Epeak of the 1 s peak spectra were larger, i.e., the spectra were harder, than the total fluence spectra. Spectral simulations based on Fermi-GBM results suggest that the higher Epeaks measured by the Suzaku WAM could be due to detector selection bias, mainly caused by the limited energy range above 100 keV.
  Scientific journal
  DOI：https://doi.org/10.1093/pasj/psz054
  Scopus：https://www.scopus.com/inward/record.uri?partnerID=HzOxMe3b&scp=85070829907&origin=inward
  Scopus Citedby：https://www.scopus.com/inward/citedby.uri?partnerID=HzOxMe3b&scp=85070829907&origin=inward
  DOI ID：10.1093/pasj/psz054, ISSN：0004-6264, eISSN：2053-051X, SCOPUS ID：85070829907
• ALMA Polarimetry of AT2018cow　　　　　　　　　　　　　　　
  Kuiyun Huang; Jiro Shimoda; Yuji Urata; Kenji Toma; Kazutaka Yamaoka; Keiichi Asada; Hiroshi Nagai; Satoko Takahashi; Glen Petitpas; Makoto Tashiro
  The Astrophysical Journal, Volume：878, Number：1, Jun. 2019, [Reviewed]
  We present the first radio polarimetric observations of a fast-rising blue optical transient, AT2018cow. Two epochs of polarimetry with additional coincident photometry were performed with the Atacama Large Millimeter/submillimeter Array. The overall photometric results based on simultaneous observations in the 100 and 230 GHz bands are consistent with the nonthermal radiation model reported by Ho et al. and indicate that the spectral peaks (similar to 110 GHz at the first epoch and similar to 67 GHz at the second epoch) represent the synchrotron self-absorption frequency. The non-detection of linear polarization with <0.15% in the 230 GHz band at the phase when the effect of synchrotron self-absorption was quite small in the band may be explained by internal Faraday depolarization with high circumburst density and strong magnetic field. This result supports the stellar explosion scenario rather than the tidal disruption model. The maximum energy of accelerating particles at the shocks of AT2018cow-like objects is also discussed.
  American Astronomical Society, English, Scientific journal
  DOI：https://doi.org/10.3847/2041-8213/ab23fd
  DOI ID：10.3847/2041-8213/ab23fd, ISSN：2041-8205, eISSN：2041-8213, ORCID：58996542, Web of Science ID：WOS:000471334300003
• In-Orbit Performance of the Digital Electronics for the X-Ray Microcalorimeter Onboard the Hitomi Satellite　　　　　　　　　　　　　　　
  M. Tsujimoto; M. S. Tashiro; Y. Ishisaki; S. Yamada; H. Seta; K. Mitsuda; K. R. Boyce; M. E. Eckart; C. A. Kilbourne; M. A. Leutenegger; F. S. Porter; R. L. Kelley
  Journal of Low Temperature Physics, First page：1, Last page：7, Mar. 2018, [Reviewed]
  The pulse shape processor is the onboard digital electronics unit of the X-ray microcalorimeter instrument—the soft X-ray spectrometer—onboard the Hitomi satellite. It processes X-ray events using the optimum filtering with limited resources. It was operated for 36 days in orbit continuously without issues and met the requirement of processing a (Formula presented.) event rate during the observation of bright sources. Here, we present the results obtained in orbit, focusing on its performance as the onboard digital signal processing unit of an X-ray microcalorimeter.
  Springer New York LLC, English, Scientific journal
  DOI：https://doi.org/10.1007/s10909-018-1861-z
  DOI ID：10.1007/s10909-018-1861-z, ISSN：1573-7357, SCOPUS ID：85043357531
• Performance of the helium dewar and the cryocoolers of the Hitomi soft x-ray spectrometer
  Ryuichi Fujimoto; Yoh Takei; Kazuhisa Mitsuda; Noriko Y. Yamasaki; Masahiro Tsujimoto; Shu Koyama; Kumi Ishikawa; Hiroyuki Sugita; Yoichi Sato; Keisuke Shinozaki; Atsushi Okamoto; Shunji Kitamoto; Akio Hoshino; Kosuke Sato; Yuichiro Ezoe; Yoshitaka Ishisaki; Shinya Yamada; Hiromi Seta; Takaya Ohashi; Toru Tamagawa; Hirofumi Noda; Makoto Sawada; Makoto Tashiro; Yoichi Yatsu; Ikuyuki Mitsuishi; Kenichi Kanao; Seiji Yoshida; Mikio Miyaoka; Shoji Tsunematsu; Kiyomi Otsuka; Katsuhiro Narasaki; Michael J. DiPirro; Peter J. Shirron; Gary A. Sneiderman; Caroline A. Kilbourne; Frederick Scott Porter; Meng P. Chiao; Megan E. Eckart
  Journal of Astronomical Telescopes, Instruments, and Systems, Volume：4, Number：1, Jan. 2018
  The soft x-ray spectrometer (SXS) was a cryogenic high-resolution x-ray spectrometer onboard the Hitomi (ASTRO-H) satellite that achieved energy resolution of 5 eV at 6 keV, by operating the detector array at 50 mK using an adiabatic demagnetization refrigerator (ADR). The cooling chain from room temperature to the ADR heat sink was composed of two-stage Stirling cryocoolers, a 4He Joule-Thomson cryocooler, and superfluid liquid helium and was installed in a dewar. It was designed to achieve a helium lifetime of more than 3 years with a minimum of 30 L. The satellite was launched on February 17, 2016, and the SXS worked perfectly in orbit, until March 26 when the satellite lost its function. It was demonstrated that the heat load on the helium tank was about 0.7 mW, which would have satisfied the lifetime requirement. This paper describes the design, results of ground performance tests, prelaunch operations, and initial operation and performance in orbit of the flight dewar and the cryocoolers.
  SPIE, English, Scientific journal
  DOI：https://doi.org/10.1117/1.JATIS.4.1.011208
  DOI ID：10.1117/1.JATIS.4.1.011208, ISSN：2329-4221, SCOPUS ID：85040450342
• In-flight calibration of Hitomi Soft X-ray Spectrometer. (1) Background　　　　　　　　　　　　　　　
  Kilbourne, C.A.; Sawada, M.; Tsujimoto, M.; Angellini, L.; Boyce, K.R.; Eckart, M.E.; Fujimoto, R.; Ishisaki, Y.; Kelley, R.L.; Koyama, S.; Leutenegger, M.A.; Loewenstein, M.; McCammon, D.; Mitsuda, K.; Nakashima, S.; Porter, F.S.; Seta, H.; Takei, Y.; Tashiro, M.S.; Terada, Y.; Yamada, S.; Yamasaki, N.Y.
  Publications of the Astronomical Society of Japan, Volume：70, Number：2, 2018, [Reviewed]
  The X-Ray Spectrometer (XRS) instrument of Suzaku provided the first measurement of the non-X-ray background (NXB) of an X-ray calorimeter spectrometer, but the data set was limited. The Soft X-ray Spectrometer (SXS) instrument of Hitomi was able to provide a more detailed picture of X-ray calorimeter background, with more than 360 ks of data while pointed at the Earth, and a comparable amount of blank-sky data. These data are important not only for analyzing SXS science data, but also for categorizing the contributions to the NXB in X-ray calorimeters as a class. In this paper, we present the contributions to the SXS NXB, the types and effectiveness of the screening, the interaction of the screening with the broad-band redistribution, and the residual background spectrum as a function of magnetic cut-off rigidity. The orbit-averaged SXS NXB in the range 0.3-12 keV was 4 x 10(-2) counts s(-1) cm(-2). This very low background in combination with groundbreaking spectral resolution gave SXS unprecedented sensitivity to weak spectral lines.
  OXFORD UNIV PRESS, English, Scientific journal
  DOI：https://doi.org/10.1093/pasj/psx139
  DOI ID：10.1093/pasj/psx139, ISSN：0004-6264, eISSN：2053-051X, ORCID：66394470, SCOPUS ID：85071379893, Web of Science ID：WOS:000432287600010
• In-flight performance of the soft x-ray spectrometer detector system on Astro-H
  Frederick S. Porter; Kevin R. Boyce; Meng P. Chiao; Megan E. Eckart; Ryuichi Fujimoto; Yoshitaka Ishisaki; Caroline Anne Kilbourne; Maurice A. Leutenegger; Daniel McCammon; Kazuhisa Mitsuda; Kosuke Sato; Hiromi Seta; Makoto Sawada; Gary A. Sneiderman; Andrew E. Szymkowiak; Yoh Takei; Makoto S. Tashiro; Masahiro Tsujimoto; Tomomi Watanabe; Shinya Yamada
  Journal of Astronomical Telescopes, Instruments, and Systems, Volume：4, Number：1, First page：011218, Jan. 2018, [Reviewed]
  The soft x-ray spectrometer (SXS) instrument was launched aboard the Astro-H (Hitomi) observatory on February 17, 2016. The SXS is based on a high-sensitivity x-ray calorimeter detector system that has been successfully deployed in many ground and suborbital spectrometers. The instrument was to provide essential diagnostics for nearly every class of x-ray emitting objects from the atmosphere of Jupiter to the outskirts of galaxy clusters, without degradation for spatially extended objects. The SXS detector system consisted of a 36-pixel cryogenic microcalorimeter array operated at a heat sink temperature of 50 mK. In preflight testing, the detector system demonstrated a resolving power of better than 1300 at 6 keV with a simultaneous bandpass from below 0.3 keV to above 12 keV with a timing precision better than 100 μs. In addition, a solid-state anticoincidence detector was placed directly behind the detector array for background suppression. The detector error budget included the measured interference from the SXS cooling system and the spacecraft. Additional margin for on-orbit gain stability and on-orbit spacecraft interference were also included predicting an on-orbit performance that meets or exceeds the 7-eV FWHM at 6-keV requirement. The actual on-orbit spectral resolution was better than 5 eV FWHM at 6 keV, easily satisfying the instrument requirement. Here, we discuss the actual on-orbit performance of the SXS detector system and compare this to performance in preflight testing and the on-orbit predictions. We will also discuss the on-orbit gain stability, additional on-orbit interference, and measurements of the on-orbit background.
  SPIE, English, Scientific journal
  DOI：https://doi.org/10.1117/1.JATIS.4.1.011218
  DOI ID：10.1117/1.JATIS.4.1.011218, ISSN：2329-4221, SCOPUS ID：85042601972
• Time assignment system and its performance aboard the Hitomi satellite　　　　　　　　　　　　　　　
  Yukikatsu Terada; Sunao Yamaguchi; Shigenobu Sugimoto; Taku Inoue; Souhei Nakaya; Maika Murakami; Seiya Yabe; Kenya Oshimizu; Mina Ogawa; Tadayasu Dotani; Yoshitaka Ishisaki; Kazuyo Mizushima; Takaashi Kominato; Hiroaki Mine; Hiroki Hihara; Kaori Iwase; Tomomi Kouzu; Makoto S. Tashiro; Chikara Natsukari; Masanobu Ozaki; Motohide Kokubun; Tadayuki Takahashi; Satoko Kawakami; Masaru Kasahara; Susumu Kumagai; Lorella Angelini; Michael Witthoeft
  JOURNAL OF ASTRONOMICAL TELESCOPES INSTRUMENTS AND SYSTEMS, Volume：4, Number：1, Jan. 2018, [Reviewed]
  Fast timing capability in x-ray observation of astrophysical objects is one of the key properties for the ASTRO-H (Hitomi) mission. Absolute timing accuracies of 350 or 35 mu s are required to achieve nominal scientific goals or to study fast variabilities of specific sources. The satellite carries a GPS receiver to obtain accurate time information, which is distributed from the central onboard computer through the large and complex SpaceWire network. The details of the time system on the hardware and software design are described. In the distribution of the time information, the propagation delays and jitters affect the timing accuracy. Six other items identified within the timing system will also contribute to absolute time error. These error items have been measured and checked on ground to ensure the time error budgets meet the mission requirements. The overall timing performance in combination with hardware performance, software algorithm, and the orbital determination accuracies, etc. under nominal conditions satisfies the mission requirements of 35 mu s. This work demonstrates key points for space-use instruments in hardware and software designs and calibration measurements for fine timing accuracy on the order of microseconds for midsized satellites using the SpaceWire (IEEE1355) network. (c) The Authors. Published by SPIE under a Creative Commons Attribution 3.0 Unported License.
  SPIE-SOC PHOTO-OPTICAL INSTRUMENTATION ENGINEERS, English, Scientific journal
  DOI：https://doi.org/10.1117/1.JATIS.4.1.011206
  DOI ID：10.1117/1.JATIS.4.1.011206, ISSN：2329-4124, eISSN：2329-4221, Web of Science ID：WOS:000429569000012
• In-orbit operation of the soft x-ray spectrometer onboard the Hitomi satellite　　　　　　　　　　　　　　　
  Masahiro Tsujimoto; Kazuhisa Mitsuda, Richard; L. Kelley; Jan Willem; Den Herder; Thomas G. Bialas; Kevin R. Boyce; Meng P. Chiao; Meng P. Chiao; Cor P. De Vries; Michael J. Dipirro; Megan E. Eckart; Yuichiro Ezoe; Ryuichi Fujimoto; Akio Hoshino; Kumi Ishikawa; Yoshitaka Ishisaki; Caroline A. Kilbourne; Shu Koyama; Maurice A. Leutenegger; Maurice A. Leutenegger; Candace M. Masters; Ikuyuki Mitsuishi; Hirofumi Noda; Takashi Okajima; Atsushi Okamoto; Frederic S. Porter; Kosuke Sato; Yohichi Sato; Joseph C. Savinell; Makoto Sawada; Hiromi Seta; Peter J. Shirron; Gary A. Sneiderman; Yoh Takei; Toru Tamagawa; Makoto S. Tashiro; Tomomi Watanabe; Shinya Yamada; Noriko Y. Yamasaki; Yoichi Yatsu
  Journal of Astronomical Telescopes, Instruments, and Systems, Volume：4, Number：1, Jan. 2018, [Reviewed]
  © The Authors. Published by SPIE under a Creative Commons Attribution 3.0 Unported License. We summarize all of the in-orbit operations of the soft x-ray spectrometer (SXS) onboard the ASTRO-H (Hitomi) satellite. The satellite was launched on February 17, 2016, and the communication with the satellite ceased on March 26, 2016. The SXS was still in the commissioning phase, in which the set-ups were progressively changed. This paper is intended to serve as a concise reference of the events in orbit in order to properly interpret the SXS data taken during its short lifetime and as a test case for planning the in-orbit operation for future microcalorimeter missions.
  SPIE-SOC PHOTO-OPTICAL INSTRUMENTATION ENGINEERS, English, Scientific journal
  DOI：https://doi.org/10.1117/1.JATIS.4.1.011205
  DOI ID：10.1117/1.JATIS.4.1.011205, ISSN：2329-4124, eISSN：2329-4221, SCOPUS ID：85034817322, Web of Science ID：WOS:000429569000011
• Ground calibration of the Astro-H (Hitomi) soft x-ray spectrometer
  Eckart M.E; Adams J.S; Boyce K.R; Brown G.V; Chiao M.P; Fujimoto R; Haas D; Den Herder J.-W; Hoshino A; Ishisaki Y; Kilbourne C.A; Kitamoto S; Leutenegger M.A; McCammon D; Mitsuda K; Porter F.S; Sato K; Sawada M; Seta H; Sneiderman G.A; Szymkowiak A.E; Takei Y; Tashiro M.S; Tsujimoto M; De Vries C.P; Watanabe T; Yamada S; Yamasaki N.Y
  Journal of Astronomical Telescopes, Instruments, and Systems, Volume：4, Number：2, 2018, [Reviewed]
  DOI：https://doi.org/10.1117/1.JATIS.4.2.021406
  DOI ID：10.1117/1.JATIS.4.2.021406, ORCID：49169942, SCOPUS ID：85044623117
• In-flight performance of pulse-processing system of the ASTRO-H/Hitomi soft x-ray spectrometer
  Ishisaki Y; Yamada S; Seta H; Tashiro M; Takeda S
  Journal of Astronomical Telescopes, Instruments, and Systems, Volume：vol.4, First page：011217, Jan. 2018, [Reviewed]
  DOI：https://doi.org/10.1117/1.JATIS.4.1.011217
  DOI ID：10.1117/1.JATIS.4.1.011217
• Mid-infrared Excess from the West Hot Spot of the Radio Galaxy Pictor A Unveiled byWISE
  Naoki Isobe; Shoko Koyama; Motoki Kino; Takehiko Wada; Takao Nakagawa; Hideo Matsuhara; Kotaro Niinuma; Makoto Tashiro
  The Astrophysical Journal, Volume：850, Number：2, First page：193, Last page：193, Dec. 2017, [Reviewed]
  American Astronomical Society, Scientific journal
  DOI：https://doi.org/10.3847/1538-4357/aa94c9
  DOI ID：10.3847/1538-4357/aa94c9, eISSN：1538-4357
• Suzaku Wide-band All-sky Monitor (WAM) observations of GRBs and SGRs　　　　　　　　　　　　　　　
  Kazutaka Yamaoka; Masanori Ohno; Makoto S. Tashiro; Kevin Hurley; Hans A. Krimm; Amy Y. Lien; Norisuke Ohmori; Satoshi Sugita; Yuji Urata; Tetsuya Yasuda; Junichi Enomoto; Takeshi Fujinuma; Yasushi Fukazawa; Yoshitaka Hanabata; Wataru Iwakiri; Takafumi Kawano; Ryuuji Kinoshita; Motohide Kokubun; Kazuo Makishima; Shunsuke Matsuoka; Tsutomu Nagayoshi; Yujin Nakagawa; Souhei Nakaya; Kazuhiro Nakazawa; Yusuke Nishioka; Takanori Sakamoto; Tadayuki Takahashi; Sawako Takeda; Yukikatsu Terada; Seiya Yabe; Makoto Yamauchi; Hiraku Yoshida
  PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN, Volume：69, Number：3, Jun. 2017, [Reviewed]
  We will review results for gamma-ray bursts (GRBs) and soft gamma repeaters (SGRs), obtained from the Suzaku Wide-band All-sky Monitor (WAM) which operated for about 10 years from 2005 to 2015. The WAM is a BGO (bismuth germanate: Bi4Ge3O12) lateral shield for the Hard X-ray Detector (HXD),used mainly for rejecting its detector background, but it also works as an all-sky monitor for soft gamma-ray transients in the 50-5000 keV range thanks to its large effective area (similar to 600 cm(2) at 1MeV for one detector) and wide field of view (about half of the entire sky). The WAM actually detected more than 1400 GRBs and 300 bursts from SGRs, and this detection number is comparable to that of other GRB-specific instruments. Based on the 10 years of operation, we describe timing and spectral performance for short GRBs, weak GRBs with high redshifts, and time-resolved pulses with good statistics.
  OXFORD UNIV PRESS, English
  DOI：https://doi.org/10.1093/pasj/psx026
  DOI ID：10.1093/pasj/psx026, ISSN：0004-6264, eISSN：2053-051X, Web of Science ID：WOS:000404642800004
• Hard X-ray spectral investigations of gamma-ray bursts 120521C and 130606A at high-redshift z ∼ 6　　　　　　　　　　　　　　　
  T. Yasuda; Y. Urata; J. Enomoto; M. S. Tashiro
  Monthly Notices of the Royal Astronomical Society, Volume：466, Number：4, First page：4558, Last page：4567, May 2017
  This study presents a temporal and spectral analysis of the prompt emission of two high-redshift gamma-ray bursts (GRBs), 120521C at z ∼ 6 and 130606A at z ∼ 5.91, using data obtained from the Swift-XRT/BAT and the Suzaku-WAM simultaneously. Based on followup XRT observations, the longest durations of the prompt emissions were approximately 80 s (120521C) and 360 s (130606A) in the rest-frames of the two GRBs. These objects are thus categorized as long-duration GRBs
  however, the durations are short compared with the predicted duration of GRBs originating from first-generation stars. Because of the wide bandpass of the instruments, covering the ranges 15 keV-5 MeV (BAT-WAM) and 0.3 keV-5.0 MeV (XRT-BAT-WAM), we could successfully determine the νFν peak energies Epeaksrc in the rest-frame and isotropic-equivalent radiated energies Eiso
  Epeaksrc = 682+−845207 keV and Eiso = (8.25+−212496) × 1052 erg for 120521C, and Epeaksrc = 1209+−553304 keV and Eiso = (2.82+−001771) × 1053 erg for 130606A. These obtained characteristic parameters are in accordance with the well-known relationship between Epeaksrc and Eiso (Amati relationship). In addition, we examined the relationships between Epeaksrc and the 1-s peak luminosity, Lp, and between Epeaksrc and the geometrical corrected radiated energy, Eγ, and confirmed the Epeaksrc -Lp (Yonetoku) and Epeaksrc -Eγ (Ghirlanda) relationships. The results imply that these high-redshift GRBs at z ∼ 6, which are expected to have radiated during the reionization epoch, have properties similar to those of low-redshift GRBs regarding X-ray prompt emission.
  Oxford University Press, English, Scientific journal
  DOI：https://doi.org/10.1093/mnras/stw3130
  DOI ID：10.1093/mnras/stw3130, ISSN：1365-2966, SCOPUS ID：85021451008
• The InterPlanetary Network Supplement to the Second Fermi GBM Catalog of Cosmic Gamma-Ray Bursts　　　　　　　　　　　　　　　
  K. Hurley; R. L. Aptekar; S. V. Golenetskii; D. D. Frederiks; D. S. Svinkin; V. D. Pal'shin; M. S. Briggs; C. Meegan; V. Connaughton; J. Goldsten; W. Boynton; C. Fellows; K. Harshman; I. G. Mitrofanov; D. V. Golovin; A. S. Kozyrev; M. L. Litvak; A. B. Sanin; A. Rau; A. von Kienlin; X. Zhang; K. Yamaoka; Y. Fukazawa; M. Ohno; M. Tashiro; Y. Terada; S. Barthelmy; T. Cline; N. Gehrels; J. Cummings; H. A. Krimm; D. M. Smith; E. Del Monte; M. Feroci; M. Marisaldi
  ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES, Volume：229, Number：2, Apr. 2017, [Reviewed]
  InterPlanetary Network (IPN) data are presented for the gamma-ray bursts in the second Fermi Gamma-Ray Burst Monitor (GBM) catalog. Of the 462 bursts in that catalog between 2010 July 12 and 2012 July 11, 428, or 93%, were observed by at least 1 other instrument in the 9-spacecraft IPN. Of the 428, the localizations of 165 could be improved by triangulation. For these bursts, triangulation gives one or more annuli whose half-widths vary between about 2 3 degrees and 16 degrees, depending on the peak flux, fluence, time history, arrival direction, and the distance between the spacecraft. We compare the IPN localizations with the GBM 1s, 2s, and 3s error contours and find good agreement between them. The IPN 3s error boxes have areas between about 8 square arcminutes and 380 square degrees, and are an average of 2500 times smaller than the corresponding GBM 3s localizations. We identify four bursts in the IPN/ GBM sample whose origins were given as "uncertain," but may in fact be cosmic. This leads to an estimate of over 99% completeness for the GBM catalog.
  IOP PUBLISHING LTD, English, Scientific journal
  DOI：https://doi.org/10.3847/1538-4365/229/2/31
  DOI ID：10.3847/1538-4365/229/2/31, ISSN：0067-0049, eISSN：1538-4365, Web of Science ID：WOS:000398181000013
• Temporal Gain Correction for X-ray Calorimeter Spectrometers　　　　　　　　　　　　　　　
  F. S. Porter; M. P. Chiao; M. E. Eckart; R. Fujimoto; Y. Ishisaki; R. L. Kelley; C. A. Kilbourne; M. A. Leutenegger; D. McCammon; K. Mitsuda; M. Sawada; A. E. Szymkowiak; Y. Takei; M. Tashiro; M. Tsujimoto; T. Watanabe; S. Yamada
  JOURNAL OF LOW TEMPERATURE PHYSICS, Volume：184, Number：1-2, First page：498, Last page：504, Jul. 2016, [Reviewed]
  Calorimetric X-ray detectors are very sensitive to their environment. The boundary conditions can have a profound effect on the gain including heat sink temperature, the local radiation temperature, bias, and the temperature of the readout electronics. Any variation in the boundary conditions can cause temporal variations in the gain of the detector and compromise both the energy scale and the resolving power of the spectrometer. Most production X-ray calorimeter spectrometers, both on the ground and in space, have some means of tracking the gain as a function of time, often using a calibration spectral line. For small gain changes, a linear stretch correction is often sufficient. However, the detectors are intrinsically non-linear and often the event analysis, i.e., shaping, optimal filters etc., add additional non-linearity. Thus for large gain variations or when the best possible precision is required, a linear stretch correction is not sufficient. Here, we discuss a new correction technique based on non-linear interpolation of the energy-scale functions. Using Astro-H/SXS calibration data, we demonstrate that the correction can recover the X-ray energy to better than 1 part in 10 over the entire spectral band to above 12 keV even for large-scale gain variations. This method will be used to correct any temporal drift of the on-orbit per-pixel gain using on-board calibration sources for the SXS instrument on the Astro-H observatory.
  SPRINGER/PLENUM PUBLISHERS, English, Scientific journal
  DOI：https://doi.org/10.1007/s10909-016-1503-2
  DOI ID：10.1007/s10909-016-1503-2, ISSN：0022-2291, eISSN：1573-7357, Web of Science ID：WOS:000378689800078
• Suzaku Wide-band All-sky Monitor measurements of duration distributions of gamma-ray bursts　　　　　　　　　　　　　　　
  Ohmori, Norisuke; Yamaoka, Kazutaka; Ohno, Masanori; Sugita, Satoshi; Kinoshita, Ryuuji; Nishioka, Yusuke; Hurley, Kevin; Hanabata, Yoshitaka; Tashiro; Makoto S; Enomoto, Junichi; Fujinuma, Takeshi; Fukazawa, Yasushi; Iwakiri, Wataru; Kawano, Takafumi; Kokubun, Motohide; Makishima, Kazuo; Matsuoka, Shunsuke; Nagayoshi, Tsutomu; Nakagawa, Yujin E; Nakaya, Souhei; Nakazawa, Kazuhiro; Takahashi, Tadayuki; Takeda, Sawako; Terada, Yukikatsu; Urata, Yuji; Yabe, Seiya; Yasuda, Tetsuya; Yamauchi, Makoto
  PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN, Volume：68, Jun. 2016, [Reviewed]
  We report on the T-90 and T-50 duration distributions and their relations with spectral hardness using 1464 gamma-ray bursts (GRBs), which were observed by the Suzaku Wide-band All-sky Monitor (WAM) from 2005 August 4 to 2010 December 29. The duration distribution is clearly bimodal in three energy ranges (50-120, 120-250, and 250-550 keV), but is unclear in the 550-5000 keV range, probably because of the limited sample size. The WAM durations decrease with energy according to a power-law index of -0.058(-0.034, +0.033). The hardness-duration relation reveals the presence of short-hard and long-soft GRBs. The short: long event ratio tends to be higher with increasing energy. We compared the WAM distribution with ones measured by eight other GRB instruments. The WAM T-90 distribution is very similar to those of INTEGRAL/SPI-ACS and Granat/PHEBUS, and least likely to match the Swift/BAT distribution. The WAM short: long event ratio (0.25:0.75) is much different from Swift/BAT (0.08:0.92), but is almost the same as CGRO/BATSE (0.25:0.75). To explain this difference for BAT, we examined three effects: BAT trigger types, energy dependence of the duration, and detection sensitivity diffe
  OXFORD UNIV PRESS, Scientific journal
  DOI：https://doi.org/10.1093/pasj/psw009
  DOI ID：10.1093/pasj/psw009, ISSN：0004-6264
• Suzaku observations of the hard X-ray spectrum of Vela Jr. (SNR RX J0852.0-4622)　　　　　　　　　　　　　　　
  Takeda, Sawako; Bamba, Aya; Terada, Yukikatsu; Tashiro; Makoto S; Katsuda, Satoru; Yamazaki, Ryo; Ohira, Yutaka; Iwakiri, Wataru
  Publications of the Astronomical Society of Japan, Volume：68, Number：SP1, First page：S10, Last page：S10, Jun. 2016, [Reviewed]
  English, Scientific journal
  DOI：https://doi.org/10.1093/pasj/psw036
  DOI ID：10.1093/pasj/psw036
• In-orbit performance of the Soft X-ray Spectrometer (SXS) onboard ASTRO-H (Hitomi)　　　　　　　　　　　　　　　
  Fujimoto R.; Mitsuda K.; Yamasaki N. Y.; Takei Y.; Tsujimoto M.; Ogawa M.; Koyama S.; Ishikawa K.; Sugita H.; Sato Y.; Shinozaki K.; Okamoto A.; Ohashi T.; Ishisaki Y.; Ezoe Y.; Yamada S.; Seta H.; Tashiro M. S.; Terada Y.; Kitamoto S.; Hoshino A.; Tamagawa T.; Sato K.; Sawada M.; Noda H.; Mitsuishi I.; Murakami H.; Ota N.; Iyomoto N.; Murakami M.; Kelley R. L.; Kilbourne C. A.; Porter F. S.; Boyce K. R.; Sneiderman G. A.; DiPirro M. J.; Shirron P. J.; Bialas T.; Eckart M. E.; Chiao M. P.; Leutenegger M. A.; Watanabe T.; Sakai K.; Brown G. V.; McCammon D.; Szymkowiak A.; Herder J. -W. den; Haas D.; Vries C. de; Costantini E.; Akamatsu H.; Paltani S.; ASTRO-H SXS team
  Meeting Abstracts of the Physical Society of Japan, Volume：71, First page：367, Last page：367, 2016
  

  2016年2月17日に打ち上げられたASTRO-H (ひとみ) 衛星に搭載された精密X線分光装置 SXS (Soft X-ray Spectrometer) は，40日弱の限られた期間ではあったが，軌道上において正常に動作し，天体のデータも取得できた．SXS の軌道上での性能について報告する．

  
  The Physical Society of Japan, Japanese
  DOI：https://doi.org/10.11316/jpsgaiyo.71.2.0_367
  DOI ID：10.11316/jpsgaiyo.71.2.0_367, CiNii Articles ID：130006246130
• Calibration of the microcalorimeter spectrometer on-board the Hitomi (Astro-H) observatory　　　　　　　　　　　　　　　
  Eckart, M. E.; Boyce, K. R.; Brown, G. V.; Chiao, M. P.; Fujimoto, R.; Haas, D.; den Herder, J. -W.; Ishisaki, Y.; Kelley, R. L.; Kilbourne, C. A.; Leutenegger, M. A.; McCammon, D.; Mitsuda, K.; Porter, F. S.; Sawada, M.; Sneiderman, G. A.; Szymkowiak, A. E.; Takei, Y.; Tashiro, M.; Tsujimoto, M.; de Vries, C. P.; Watanabe, T.; Yamada, S.; Yamasaki, N. Y.
  Review of Scientific Instruments, Volume：87, Number：11, 2016, [Reviewed]
  Scientific journal
  DOI：https://doi.org/10.1063/1.4961075
  DOI ID：10.1063/1.4961075, ORCID：33310762, Web of Science ID：WOS:000390242300055
• 21pCD-11 Status of the Soft X-ray Spectrometer (SXS) onboard ASTRO-H　　　　　　　　　　　　　　　
  Tashiro M. S.; Mitsuda k.; Yamasaki N.; Takei Y.; Tsujimoto M.; Ogawa M.; Koyama S.; Sakai K.; Sugita H.; Sato Y.; Shinozaki; Okamoto A.; Fujimoto R.; Ohashi T.; Ishisaki Y.; Ezoe Y.; Yamada S.; Seta H.; Terada Y.; Kitamoto S.; Hoshino A.; Tamagawa T.; Ishikawa K.; Noda H.; Sato K.; Ota N.; Sawada M.; Mitsuishi I.; Murakami M.; Murakami H.; Iyomoto N.; Kelley R. L.; Kilbourne C. A.; Porter F. S.; Boyce K. R.; Eckart M. E.; Chiao M. P.; Leutenegger M. A.; Brown G. V.; McCammon D.; Szymkowiak A.; Herder J. -W. den; Haas D.; Vries C. de; Costantini E.; Akamatsu H.; Paltani S.; ASTRO-H SXS team
  Meeting Abstracts of the Physical Society of Japan, Volume：71, First page：509, Last page：509, 2016
  The Physical Society of Japan (JPS), Japanese
  DOI：https://doi.org/10.11316/jpsgaiyo.71.1.0_509
  DOI ID：10.11316/jpsgaiyo.71.1.0_509, ISSN：2189-079X, CiNii Articles ID：110010056547, CiNii Books ID：AA12721570
• Performance of the helium dewar and cryocoolers of ASTRO-H SXS　　　　　　　　　　　　　　　
  Ryuichi Fujimoto; Yoh Takei; Kazuhisa Mitsuda; Noriko Y. Yamasaki; Masahiro Tsujimoto; Shu Koyama; Kumi Ishikawa; Hiroyuki Sugita; Yoichi Sato; Keisuke Shinozaki; Atsushi Okamoto; Shunji Kitamoto; Akio Hoshino; Kosuke Sato; Yuichiro Ezoe; Yoshitaka Ishisaki; Shinya Yamada; Hiromi Seta; Takaya Ohashi; Toru Tamagawa; Hirofumi Noda; Makoto Sawada; Makoto Tashiro; Yoichi Yatsu; Ikuyuki Mitsuishi; Kenichi Kanao; Seiji Yoshida; Mikio Miyaoka; Shoji Tsunematsu; Kiyomi Otsuka; Katsuhiro Narasaki; Michael J. DiPirro; Peter J. Shirron; Gary A. Sneiderman; Caroline A. Kilbourne; F. Scott Porter; Meng P. Chiao; Megan E. Eckart; Richard L. Kelley
  SPACE TELESCOPES AND INSTRUMENTATION 2016: ULTRAVIOLET TO GAMMA RAY, Volume：9905, 2016
  The Soft X-ray Spectrometer (SXS) is a cryogenic high-resolution X-ray spectrometer onboard the ASTRO-H satellite, that achieves energy resolution better than 7 eV at 6 keV, by operating the detector array at 50 mK using an adiabatic demagnetization refrigerator. The cooling chain from room temperature to the ADR heat sink is composed of 2-stage Stirling cryocoolers, a He-4 Joule-Thomson cryocooler, and superfluid liquid He, and is installed in a dewar. It is designed to achieve a helium lifetime of more than 3 years with a minimum of 30 liters. The satellite was launched on 2016 February 17, and the SXS worked perfectly in orbit, until March 26 when the satellite lost its function. It was demonstrated that the heat load on the He tank was about 0.7 mW, which would have satisfied the lifetime requirement. This paper describes the design, results of ground performance tests, prelaunch operations, and initial operation and performance in orbit of the flight dewar and cryocoolers.
  SPIE-INT SOC OPTICAL ENGINEERING, English, International conference proceedings
  DOI：https://doi.org/10.1117/12.2232933
  DOI ID：10.1117/12.2232933, ISSN：0277-786X, Web of Science ID：WOS:000387731500113
• In-flight performance of the Soft X-ray Spectrometer detector system on Astro-H　　　　　　　　　　　　　　　
  Frederick S. Porter; Kevin R. Boyce; Meng P. Chiao; Megan E. Eckart; Ryuichi Fujimoto; Yoshitaka Ishisaki; Richard L. Kelley; Caroline A. Kilbourne; Maurice A. Leutenegger; Dan McCammon; Kazuhisa Mitsuda; Kosuke Sato; Hiromi Seta; Makoto Sawada; Gary A. Sneiderman; Andrew E. Szymkowiak; Yoh Takei; Makoto S. Tashiro; Masahiro Tsujimoto; Tomomi Watanabe; Shinya Yamada
  SPACE TELESCOPES AND INSTRUMENTATION 2016: ULTRAVIOLET TO GAMMA RAY, Volume：9905, 2016
  The SXS instrument was launched aboard the Astro-H observatory on February 17, 2016. The SXS spectrometer is based on a high sensitivity x-ray calorimeter detector system that has been successfully deployed in many ground and sub-orbital spectrometers. The instrument was to provide essential diagnostics for nearly every class of x-ray emitting objects from the atmosphere of Jupiter to the outskirts of galaxy clusters, without degradation for spatially extended objects. The SXS detector system consisted of a 36-pixel cryogenic microcalorimeter array operated at a heat sink temperature of 50 mK. In pre-flight testing, the detector system demonstrated a resolving power of better than 1300 at 6 keV with a simultaneous band-pass from below 0.3 keV to above 12 keV with a timing precision better than 100 mu s. In addition, a solid-state anti-coincidence detector was placed directly behind the detector array for background suppression. The detector error budget included the measured interference from the SXS cooling system and the spacecraft. Additional margin for on-orbit gain-stability, and on-orbit spacecraft interference were also included predicting an on-orbit performance that meets or exceeds the 7 eV FWHM at 6 keV requirement. The actual on-orbit spectral resolution was better than 5 eV FWHM at 6 keV, easily satisfying the instrument requirement. Here we discuss the actual on-orbit performance of the SXS detector system and compare this to performance in pre-flight testing and the on-orbit predictions. We will also discuss the on-orbit gain stability, additional on-orbit interference, and measurements of the on-orbit background.
  SPIE-INT SOC OPTICAL ENGINEERING, English, International conference proceedings
  DOI：https://doi.org/10.1117/12.2232799
  DOI ID：10.1117/12.2232799, ISSN：0277-786X, Web of Science ID：WOS:000387731500021
• The Astro-H High Resolution Soft X-Ray Spectrometer　　　　　　　　　　　　　　　
  Richard L. Kelley; Hiroki Akamatsu; Phillipp Azzarell; Tom Bialas; Kevin R. Boyce; Gregory V. Brown; Edgar Canavan; Meng P. Chiao; Elisa Costantini; Michael J. DiPirro; Megan E. Eckart; Yuichiro Ezoe; Ryuichi Fujimoto; Daniel Haas; Jan-Willem den Herder; Akio Hoshino; Kumi Ishikawa; Yoshitaka Ishisaki; Naoko Iyomoto; Caroline A. Kilbourne; Mark Kimball; Shunji Kitamoto; Saori Konami; Shu Koyama; Maurice A. Leutenegger; Dan McCammon; Joseph Miko; Kazuhisa Mitsuda; Ikuyuki Mitsuishi; Harvey Moseley; Hiroshi Murakami; Masahide Murakami; Hirofumi Noda; Mina Ogawa; Takaya Ohashi; Atsushi Okamoto; Naomi Ota; Stephane Paltani; F. Scott Porter; Kazuhiro Sakai; Kosuke Sato; Yohichi Sato; Makoto Sawada; Hiromi Seta; Keisuke Shinozaki; Peter J. Shirron; Gary A. Sneiderman; Hiroyuki Sugita; Andrew E. Szymkowiak; Yoh Takei; Toni Tamagawa; Makoto Tashiro; Yukikatsu Terada; Masahiro Tsujimoto; Cor P. de Vries; Shinya Yamada; Noriko Y. Yamasaki; Yoichi Yatsu
  SPACE TELESCOPES AND INSTRUMENTATION 2016: ULTRAVIOLET TO GAMMA RAY, Volume：9905, 2016, [Reviewed]
  We present the overall design and performance of the Astro-H (Hitomi) Soft X-Ray Spectrometer (SXS). The instrument uses a 36-pixel array of x-ray microcalorimeters at the focus of a grazing-incidence x-ray mirror Soft X-Ray Telescope (SXT) for high-resolution spectroscopy of celestial x-ray sources. The instrument was designed to achieve an energy resolution better than 7 eV over the 0.3-12 keV energy range and operate for more than 3 years in orbit. The actual energy resolution of the instrument is 4-5 eV as demonstrated during extensive ground testing prior to launch and in orbit. The measured mass flow rate of the liquid helium cryogen and initial fill level at launch predict a lifetime of more than 4 years assuming steady mechanical cooler performance. Cryogen-free operation was successfully demonstrated prior to launch. The successful operation of the SXS in orbit, including the first observations of the velocity structure of the Perseus cluster of galaxies, demonstrates the viability and power of this technology as a tool for astrophysics.
  SPIE-INT SOC OPTICAL ENGINEERING, English, International conference proceedings
  DOI：https://doi.org/10.1117/12.2232509
  DOI ID：10.1117/12.2232509, ISSN：0277-786X, eISSN：1996-756X, SCOPUS ID：85003530545, Web of Science ID：WOS:000387731500020
• In-orbit operation of the ASTRO-H SXS　　　　　　　　　　　　　　　
  Masahiro Tsujimoto; Kazuhisa Mitsuda; Richard L. Kelley; Jan-Willem A. den Herder; Hiroki Akamatsu; Thomas G. Bialas; Kevin R. Boyce; Gregory V. Brown; Meng P. Chiao; Elisa Costantini; Cor P. de Vries; Michael J. DiPirro; Megan E. Eckart; Yuichiro Ezoe; Ryuichi Fujimoto; Daniel Haas; Akio Hoshino; Kumi Ishikawa; Yoshitaka Ishisaki; Naoko Iyomoto; Caroline A. Kilbourne; Shunji Kitamoto; Shu Koyama; Maurice A. Leutenegger; Dan McCammon; Ikuyuki Mitsuishi; Hiroshi Murakami; Masahide Murakami; Hirofumi Noda; Mina Ogawa; Naomi Ota; Stephane Paltani; Frederick S. Porter; Kosuke Sato; Yoichi Sato; Makoto Sawada; Hiromi Seta; Keisuke Shinozaki; Peter J. Shirron; Gary A. Sneiderman; Hiroyuki Sugita; Andrew E. Szymkowiak; Yoh Takei; Toru Tamagawa; Makoto S. Tashiro; Yukikatsu Terada; Shinya Yamada; Noriko Y. Yamasaki; Yoichi Yatsu
  SPACE TELESCOPES AND INSTRUMENTATION 2016: ULTRAVIOLET TO GAMMA RAY, Volume：9905, 2016, [Reviewed]
  We summarize all the in-orbit operations of the Soft X-ray Spectrometer (SXS) onboard the ASTRO-H (Hitomi) satellite. The satellite was launched on 2016/02/17 and the communication with the satellite ceased on 2016/03/26. The SXS was still in the commissioning phase, in which the setups were progressively changed. This article is intended to serve as a reference of the events in the orbit to properly interpret the SXS data taken during its short life time, and as a test case for planning the in-orbit operation for future micro-calorimeter missions.
  SPIE-INT SOC OPTICAL ENGINEERING, English, International conference proceedings
  DOI：https://doi.org/10.1117/12.2231784
  DOI ID：10.1117/12.2231784, ISSN：0277-786X, eISSN：1996-756X, Web of Science ID：WOS:000387731500023
• A missing-link in the supernova-GRB connection: The case of SN 2012ap　　　　　　　　　　　　　　　
  Sayan Chakraborti; Alicia Soderberg; Laura Chomiuk; Atish Kamble; Naveen Yadav; Alak Ray; Kevin Hurley; Raffaella Margutti; Dan Milisavljevic; Michael Bietenholz; Andreas Brunthaler; Giuliano Pignata; Elena Pian; Paolo Mazzali; Claes Fransson; Norbert Bartel; Mario Hamuy; Emily Levesque; Andrew Macfadyen; Jason Dittmann; Miriam Krauss; M. S. Briggs; V. Connaughton; K. Yamaoka; T. Takahashi; M. Ohno; Y. Fukazawa; M. Tashiro; Y. Terada; T. Murakami; J. Goldsten; S. Barthelmy; N. Gehrels; J. Cummings; H. Krimm; D. Palmer; S. Golenetskii; R. Aptekar; D. Frederiks; D. Svinkin; T. Cline; I. G. Mitrofanov; D. Golovin; M. L. Litvak; A. B. Sanin; W. Boynton; C. Fellows; K. Harshman; H. Enos; A. Von Kienlin; A. Rau; X. Zhang; V. Savchenko
  Astrophysical Journal, Volume：805, Number：2, Jun. 2015
  Gamma-ray bursts (GRBs) are characterized by ultra-relativistic outflows, while supernovae are generally characterized by non-relativistic ejecta. GRB afterglows decelerate rapidly, usually within days, because their low-mass ejecta rapidly sweep up a comparatively larger mass of circumstellar material. However, supernovae with heavy ejecta can be in nearly free expansion for centuries. Supernovae were thought to have non-relativistic outflows except for a few relativistic ones accompanied by GRBs. This clear division was blurred by SN 2009bb, the first supernova with a relativistic outflow without an observed GRB. However, the ejecta from SN 2009bb was baryon loaded and in nearly free expansion for a year, unlike GRBs. We report the first supernova discovered without a GRB but with rapidly decelerating mildly relativistic ejecta, SN 2012ap. We discovered a bright and rapidly evolving radio counterpart driven by the circumstellar interaction of the relativistic ejecta. However, we did not find any coincident GRB with an isotropic fluence of more than one-sixth of the fluence from GRB 980425. This shows for the first time that central engines in SNe Ic, even without an observed GRB, can produce both relativistic and rapidly decelerating outflows like GRBs.
  Institute of Physics Publishing, English, Scientific journal
  DOI：https://doi.org/10.1088/0004-637X/805/2/187
  DOI ID：10.1088/0004-637X/805/2/187, ISSN：1538-4357, SCOPUS ID：84934876354
• Suzaku observation of X-ray variability in soft state LMC X-1
  Koyama S; Yamada S; Kubota A; Tashiro M; Terada Y
  Publications of the Astronomical Society of Japan, Volume：vol.67, First page：46, Jun. 2015, [Reviewed]
  DOI：https://doi.org/10.1093/pasj/psv017
  DOI ID：10.1093/pasj/psv017
• Sub-MeV band observation of a hard burst from AXP 1E 1547.0-5408 with the Suzaku Wide-band All-sky Monitor
  Yasuda T; Iwakiri W; Tashiro M; Terada Y; Kouzu T. et al; Enoto T; a; th author out o; authors
  Publications of the Astronomical Society of Japan, Volume：vol.67, First page：41, Jun. 2015, [Reviewed]
  DOI：https://doi.org/10.1093/pasj/psv011
  DOI ID：10.1093/pasj/psv011
• 23pDK-4 Development status of Soft X-ray Spectrometer (SXS) onboard ASTRO-H (VI)　　　　　　　　　　　　　　　
  Ishisaki K.; Mitsuda K.; Yamasaki N.; Takei Y.; Tsujimoto M.; Ogawa M.; Sugita H.; Sato Y.; Shinozaki K.; Okamoto A.; Fujimoto R.; Ohashi T.; Ezoe Y.; Yamada S.; Konami S.; Tashiro M.; Terada Y.; H. Seta H. Seta; Kitamoto S.; Hoshino A.; Tamagawa T.; Ishikawa K.; Noda H.; Sato K.; Ota N.; Sawada M.; Mitsuishi I.; Murakami M.; Murakami H.; Iyomoto N.; Kelley R.L.; Kilbourne C.A.; Porter F.S.; Boyce K.R.; Eckart M.E.; Chiao M.P.; Leutenegger M.A.; Brown G.V.; McCammon D.; Szymkowiak A.; Herder J.-W. den; Haas D.; de Vries C.; Costantini E.; Akamatsu H.; Paltani S.; ASTRO-H SXS team
  Meeting Abstracts of the Physical Society of Japan, Volume：70, First page：471, Last page：471, 2015
  The Physical Society of Japan (JPS), Japanese
  DOI：https://doi.org/10.11316/jpsgaiyo.70.1.0_471
  DOI ID：10.11316/jpsgaiyo.70.1.0_471, ISSN：2189-079X, CiNii Articles ID：110009990627, CiNii Books ID：AA12721570
• Optical follow-up observations of PTF10qts, a luminous broad-lined type Ic supernova found by the palomar transient factory　　　　　　　　　　　　　　　
  E. S. Walker; P. A. Mazzali; E. Pian; K. Hurley; I. Arcavi; S. B. Cenko; A. Gal-Yam; A. Horesh; M. Kasliwal; D. Poznanski; J. M. Silverman; M. Sullivan; J. S. Bloom; A. V. Filippenko; S. R. Kulkarni; P. E. Nugent; E. Ofek; S. Barthelmy; W. Boynton; J. Goldsten; S. Golenetskii; M. Ohno; M. S. Tashiro; K. Yamaoka; X. L. Zhang
  Monthly Notices of the Royal Astronomical Society, Volume：442, Number：3, First page：2768, Last page：2779, 2014
  We present optical photometry and spectroscopy of the broad-lined Type Ic supernova (SN Ic-BL) PTF10qts, which was discovered as part of the Palomar Transient Factory. The SN was located in a dwarf galaxy of magnitude r = 21.1 at a redshift z = 0.0907. We find that the R-band light curve is a poor proxy for bolometric data and use photometric and spectroscopic data to construct and constrain the bolometric light curve. The derived bolometric magnitude at maximum light is Mbol =-18.51 ± 0.2 mag, comparable to that of SN 1998bw (Mbol = -18.7 mag) which was associated with a gamma-ray burst (GRB). PTF10qts is one of the most luminous SNe Ic-BL observed without an accompanying GRB. We estimate the physical parameters of the explosion using data from our programme of follow-up observations, finding that it produced a larger mass of radioactive nickel compared to other SNe Ic-BL with similar inferred ejecta masses and kinetic energies. The progenitor of the event was likely an ~20 M⊙ star. © 2014 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society.
  Oxford University Press, English, Scientific journal
  DOI：https://doi.org/10.1093/mnras/stu1017
  DOI ID：10.1093/mnras/stu1017, ISSN：1365-2966, SCOPUS ID：84904546349
• Soft x-ray spectrometer (SXS): the high-resolution cryogenic spectrometer onboard ASTRO-H　　　　　　　　　　　　　　　
  Kazuhisa Mitsuda; Richard L. Kelley; Hiroki Akamatsu; Thomas Bialas; Kevin R. Boyce; Gregory V. Brown; Edgar Canavan; Meng Chiao; Elisa Costantini; Jan-Willem den Herder; Cor de Vries; Michael J. DiPirro; Megan E. Eckart; Yuichiro Ezoe; Ryuichi Fujimoto; Daniel Haas; Akio Hoshino; Kumi Ishikawa; Yoshitaka Ishisaki; Naoko Iyomoto; Caroline A. Kilbourne; Mark Kimball; Shunji Kitamoto; Saori Konami; Maurice A. Leutenegger; Dan McCammon; Joseph Miko; Ikuyuki Mitsuishi; Hiroshi Murakami; Masahide Murakami; Hirofumi Noda; Mina Ogawa; Takaya Ohashi; Atsushi Okamoto; Naomi Ota; Stephane Paltani; F. Scott Porter; Kosuke Sato; Yoichi Sato; Makoto Sawada; Hitomi Seta; Keisuke Shinozaki; Peter J. Shirron; Gary A. Sneiderman; Hiroyuki Sugita; Andrew Szymkowiak; Yoh Takei; Toru Tamagawa; Makoto S. Tashiro; Yukikatsu Terada; Masahiro Tsujimoto; Shinya Yamada; Noriko Y. Yamasaki
  SPACE TELESCOPES AND INSTRUMENTATION 2014: ULTRAVIOLET TO GAMMA RAY, Volume：9144, 2014, [Reviewed]
  We present the development status of the Soft X-ray Spectrometer (SXS) onboard the ASTRO-H mission. The SXS provides the capability of high energy-resolution X-ray spectroscopy of a FWHM energy resolution of < 7eV in the energy range of 0.3 - 10 keV. It utilizes an X-ray micorcalorimeter array operated at 50 mK. The SXS microcalorimeter subsystem is being developed in an EM-FM approach. The EM SXS cryostat was developed and fully tested and, although the design was generally confirmed, several anomalies and problems were found. Among them is the interference of the detector with the micro-vibrations from the mechanical coolers, which is the most difficult one to solve. We have pursued three different countermeasures and two of them seem to be effective. So far we have obtained energy resolutions satisfying the requirement with the FM cryostat.
  SPIE-INT SOC OPTICAL ENGINEERING, English, International conference proceedings
  DOI：https://doi.org/10.1117/12.2057199
  DOI ID：10.1117/12.2057199, ISSN：0277-786X, eISSN：1996-756X, Web of Science ID：WOS:000354529100070
• Performance verification and system integration tests of the pulse shape processor for the soft X-ray spectrometer onboard ASTRO-H　　　　　　　　　　　　　　　
  Sawako Takeda; Makoto S. Tashiro; Yoshitaka Ishisaki; Masahiro Tsujimoto; Hiromi Seta; Yuya Shimoda; Sunao Yamaguchi; Sho Uehara; Yukikatsu Terada; Ryuichi Fujimoto; Kazuhisa Mitsuda
  SPACE TELESCOPES AND INSTRUMENTATION 2014: ULTRAVIOLET TO GAMMA RAY, Volume：9144, 2014, [Reviewed]
  The soft X-ray spectrometer (SXS) aboard ASTRO-H is equipped with dedicated digital signal processing units called pulse shape processors (PSPs). The X-ray microcalorimeter system SXS has 36 sensor pixels, which are operated at 50 mK to measure heat input of X-ray photons and realize an energy resolution of 7 eV FWHM in the range 0.3-12.0 keV. Front-end signal processing electronics are used to filter and amplify the electrical pulse output from the sensor and for analog-to-digital conversion. The digitized pulses from the 36 pixels are multiplexed and are sent to the PSP over lowvoltage differential signaling lines. Each of two identical PSP units consists of an FPGA board, which assists the hardware logic, and two CPU boards, which assist the onboard software. The FPGA board triggers at every pixel event and stores the triggering information as a pulse waveform in the installed memory. The CPU boards read the event data to evaluate pulse heights by an optimal filtering algorithm. The evaluated X-ray photon data (including the pixel ID, energy, and arrival time information) are transferred to the satellite data recorder along with event quality information. The PSP units have been developed and tested with the engineering model (EM) and the flight model. Utilizing the EM PSP, we successfully verified the entire hardware system and the basic software design of the PSPs, including their communication capability and signal processing performance. In this paper, we show the key metrics of the EM test, such as accuracy and synchronicity of sampling clocks, event grading capability, and resultant energy resolution.
  SPIE-INT SOC OPTICAL ENGINEERING, English, International conference proceedings
  DOI：https://doi.org/10.1117/12.2055899
  DOI ID：10.1117/12.2055899, ISSN：0277-786X, Web of Science ID：WOS:000354529100162
• Design of the Time assignment System for ASTRO-H and Its Performance before Launch　　　　　　　　　　　　　　　
  Yukikatsu Terada; Sunao Yamaguchi; Shigenobu Sugimoto; Taku Inoue; Souhei Nakaya; Mina Ogawa; Tadayasu Dotani; Yoshitaka Ishisaki; Kazuyo Mizushima; Takashi Kominato; Hiroaki Mine; Hiroki Hihara; Kaori Iwase; Tomomi Kouzu; Makoto S. Tashiro; Chikara Natsukari; Masanobu Ozaki; Motohide Kokubun; Tadayuki Takahashi; Satoko Kawakami; Masan. Kasahara; Susumu Kumagai; Lorella Angelini; Michael Witthoeft
  2014 IEEE NUCLEAR SCIENCE SYMPOSIUM AND MEDICAL IMAGING CONFERENCE (NSS/MIC), 2014, [Reviewed]
  IEEE, English, International conference proceedings
  Web of Science ID：WOS:000392917500464
• Sub-MeV all sky survey with a compact Si/CdTe Compton telescope　　　　　　　　　　　　　　　
  Nakazawa, Kazuhiro; Takahashi, Tadayuki; Watanabe, Shin; Ichinohe, Yuto; Takeda, Shin'ichiro; Enoto, Teruaki; Fukazawa, Yasushi; Kamae, Tuneyoshi; Kokubun, Motohide; Makishima, Kazuo; Mitani, Takefumi; Mizuno, Tsunefumi; Nomachi, Masaharu; Tajima, Hiroyasu; Takashima, Takeshi; Tamagawa, Toru; Terada, Yukikatsu; Tashiro, Makoto; Uchiyama, Yasunobu; Yoshimitsu, Tetsuo
  SPACE TELESCOPES AND INSTRUMENTATION 2014: ULTRAVIOLET TO GAMMA RAY, Volume：9144, 2014, [Reviewed]
  Recent progress in wide field of view or all-sky observations such as Swift/BAT hard X-ray monitor and Fermi GeV gamma-ray observatory has opened up a new era of time-domain high energy astro-physics addressing new insight in, e.g., particle acceleration in the universe. MeV coverage with comparable sensitivity, i.e. 1 similar to 10 mCrab is missing and a new MeV all-sky observatory is needed. These new MeV mission tend to be large, power-consuming and hence expensive, and its realization is yet to come. A compact sub-MeV (0.2-2 MeV) all-sky mission is proposed as a path finder for such mission. It is based on a Si/CdTe semiconductor Compton telescope technology employed in the soft gamma-ray detector onboard ASTRO-H, to be launched in to orbit on late 2015. The mission is kept as small as 0.5 x 0.5 x 0.4 m(3), 150 kg in weight and 200 W in power in place of the band coverage above a few MeV, in favor of early realization as a sub-payload to other large platforms, such as the international space station.
  SPIE-INT SOC OPTICAL ENGINEERING, English, International conference proceedings
  DOI：https://doi.org/10.1117/12.2055422
  DOI ID：10.1117/12.2055422, ISSN：0277-786X, Web of Science ID：WOS:000354529100015
• Suzaku Detection of Thermal X-Ray Emission Associated with the Western Radio Lobe of Fornax A　　　　　　　　　　　　　　　
  Hiromi Seta; Makoto S. Tashiro; Susumu Inoue
  PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN, Volume：65, Number：5, Oct. 2013
  We present the results of X-ray mapping observations of the western radio lobe of the Fornax A galaxy, using the X-ray Imaging Spectrometer (XIS) onboard the Suzaku satellite with a total exposure time of 327 ks. The purpose of this study is to investigate the nature and spatial extent of the diffuse thermal emission around the lobe by exploiting the low and stable background of XIS. The diffuse thermal emission had been consistently reported in all previous studies of this region, but its physical nature and relation to the radio lobe had not been examined in detail. Using a data set covering the entire western lobe and the central galaxy NGC 1316, as well as comparison sets in the vicinity, we find convincingly the presence of thermal plasma emission with a temperature of similar to 1 keV in excess of conceivable background and contaminating emission (cosmic X-ray background, Galactic halo, intra-cluster gas of Fornax, interstellar gas of NGC 1316, and the ensemble of point-like sources). Its surface brightness is consistent with having a spherical distribution peaking at the center of the western lobe with a projected radius of similar to 12'. If the volume filling factor of the thermal gas is assumed to be unity, its estimated total mass amounts to similar to 10(10) M-circle dot, which would be similar to 10(2) times that of the central black hole, and comparable to that of the current gas mass of the host galaxy. Its energy density is comparable to or larger than those in the magnetic field and non-thermal electrons responsible for the observed radio and X-ray emission.
  OXFORD UNIV PRESS, English, Scientific journal
  DOI：https://doi.org/10.1093/pasj/65.5.106
  DOI ID：10.1093/pasj/65.5.106, ISSN：0004-6264, eISSN：2053-051X, Web of Science ID：WOS:000328300300015
• Metals in the Intracluster Medium of MS 1512.4+3647 Observed with Suzaku: Implications for the Metal Enrichment History　　　　　　　　　　　　　　　
  Yuya Shimoda; Madoka Kawaharada; Kosuke Sato; Takaya Ohashi; Yoshitaka Ishisaki; Ikuyuki Mitsuishi; Hiroki Akamatsu; Makoto S. Tashiro
  PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN, Volume：65, Number：5, Oct. 2013, [Reviewed]
  The cluster of galaxies MS 1512.4+3647 (z = 0.372) was observed with Suzaku for 270 ks. Besides the Fe abundance, the abundances of Mg, Si, S, and Ni were separately determined for the first time in a medium redshift cluster (z > 0.3). The derived abundance pattern of MS 1512.4+3647 is consistent with those of nearby clusters, suggesting that the system has similar contributions from supernovae (SNe) Ia and SNe II to nearby clusters. The number ratio of SNe II to SNe Ia is similar to 3. The estimated total numbers of both SNe II and SNe Ia against the gas mass indicate similar correlations with those for the nearby clusters. The abundance results of MS 1512.4+3647 is consistent with the standard scenario that the SN II rate history roughly follows the star-formation history, which has a peak at 1 < z < 2, and then declines by about one order of magnitude toward z similar to 0. The similar number of SNe Ia to the nearby clusters suggests that the SN Ia rate declines steeply from z = 0.37 to z = 0, and/or SN Ia explosions occurred predominantly at larger redshifts.
  OXFORD UNIV PRESS, English, Scientific journal
  DOI：https://doi.org/10.1093/pasj/65.5.111
  DOI ID：10.1093/pasj/65.5.111, ISSN：0004-6264, eISSN：2053-051X, Web of Science ID：WOS:000328300300020
• Erratum: Hard X-ray spectrum from the west lobe of radio galaxy fornax A observed with suzaku　　　　　　　　　　　　　　　
  Makoto S. Tashiro; Naoki Isobe; Hiromi Seta; Keiko Matsuta; Yuichi Yaji
  Publications of the Astronomical Society of Japan, Volume：65, Number：4, Aug. 2013, [Reviewed]
  Oxford University Press, English, Scientific journal
  DOI：https://doi.org/10.1093/pasj/65.4.94
  DOI ID：10.1093/pasj/65.4.94, ISSN：0004-6264, SCOPUS ID：84885405736
• Spectral Variation of Hard X-Ray Emission from the Crab Nebula with the Suzaku Hard X-Ray Detector　　　　　　　　　　　　　　　
  Kouzu, Tomomi; Tashiro; Makoto S; Terada, Yukikatsu; Yamada, Shin'ya; Bamba, Aya; Enoto, Teruaki; Mori, Koji; Fukazawa, Yasushi; Makishima, Kazuo
  PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN, Volume：65, Number：4, First page：74, Last page：1-11, Aug. 2013, [Reviewed]
  The Crab Nebula is one of the brightest and most stable sources in the X-ray sky. Year-scale flux variation from the object was recently revealed in the hard X-ray band by four satellites. This marked the first detection of year-scale variability from pulsar wind nebulae in the hard X-ray band. The Crab Nebula has been observed at least once a year for calibration purposes with the Suzaku Hard X-ray Detector (HXD) since its launch in 2005. In order to investigate possible spectral changes as well as flux variation, archival data of the HXD were analyzed. The flux variation reported by other instruments was confirmed in the 25-100 keV band by the HXD at a few percent level, but flux above 100 keV did not follow the trend in variation below 100 keV. The hardness ratios produced utilizing the PIN and GSO sensors installed in the HXD exhibit significant scattering, thereby indicating spectral variations in the hard X-ray band. The spectral changes were quantified by spectral fitting with a broken power-law model. The difference between the two photon indexes of the broken power-law model in harder and softer energy bands is in the range of < 2.54. Taking into account a flux variation o
  ASTRONOMICAL SOC JAPAN, English, Scientific journal
  ISSN：0004-6264, CiNii Articles ID：40020043177, CiNii Books ID：AA1082896X
• Interplanetary network localizations of konus short gamma-ray bursts　　　　　　　　　　　　　　　
  V. D. Pal'Shin; K. Hurley; D. S. Svinkin; R. L. Aptekar; S. V. Golenetskii; D. D. Frederiks; E. P. Mazets; P. P. Oleynik; M. V. Ulanov; T. Cline; I. G. Mitrofanov; D. V. Golovin; A. S. Kozyrev; M. L. Litvak; A. B. Sanin; W. Boynton; C. Fellows; K. Harshman; J. Trombka; T. McClanahan; R. Starr; J. Goldsten; R. Gold; A. Rau; A. Von Kienlin; V. Savchenko; D. M. Smith; W. Hajdas; S. D. Barthelmy; J. Cummings; N. Gehrels; H. Krimm; D. Palmer; K. Yamaoka; M. Ohno; Y. Fukazawa; Y. Hanabata; T. Takahashi; M. Tashiro; Y. Terada; T. Murakami; K. Makishima; M. S. Briggs; R. M. Kippen; C. Kouveliotou; C. Meegan; G. Fishman; V. Connaughton; M. Boër; C. Guidorzi; F. Frontera; E. Montanari; F. Rossi; M. Feroci; L. Amati; L. Nicastro; M. Orlandini; E. Del Monte; E. Costa; I. Donnarumma; Y. Evangelista; I. Lapshov; F. Lazzarotto; L. Pacciani; M. Rapisarda; P. Soffitta; G. Di Cocco; F. Fuschino; M. Galli; C. Labanti; M. Marisaldi; J. L. Atteia; R. Vanderspek; G. Ricker
  Astrophysical Journal, Supplement Series, Volume：207, Number：2, Aug. 2013
  Between the launch of the Global Geospace Science Wind spacecraft in 1994 November and the end of 2010, the Konus-Wind experiment detected 296 short-duration gamma-ray bursts (including 23 bursts which can be classified as short bursts with extended emission). During this period, the Interplanetary Network (IPN) consisted of up to 11 spacecraft, and using triangulation, the localizations of 271 bursts were obtained. We present the most comprehensive IPN localization data on these events. The short burst detection rate, ∼18 yr-1, exceeds that of many individual experiments. © 2013. The American Astronomical Society. All rights reserved.
  English, Scientific journal
  DOI：https://doi.org/10.1088/0067-0049/207/2/38
  DOI ID：10.1088/0067-0049/207/2/38, ISSN：0067-0049, SCOPUS ID：84881150740
• THE INTERPLANETARY NETWORK SUPPLEMENT TO THE FERMI GBM CATALOG OF COSMIC GAMMA-RAY BURSTS　　　　　　　　　　　　　　　
  K. Hurley; V. D. Pal'shin; R. L. Aptekar; S. V. Golenetskii; D. D. Frederiks; E. P. Mazets; D. S. Svinkin; M. S. Briggs; V. Connaughton; C. Meegan; J. Goldsten; W. Boynton; C. Fellows; K. Harshman; I. G. Mitrofanov; D. V. Golovin; A. S. Kozyrev; M. L. Litvak; A. B. Sanin; A. Rau; A. von Kienlin; X. Zhang; K. Yamaoka; Y. Fukazawa; Y. Hanabata; M. Ohno; T. Takahashi; M. Tashiro; Y. Terada; T. Murakami; K. Makishima; S. Barthelmy; T. Cline; N. Gehrels; J. Cummings; H. A. Krimm; D. M. Smith; E. Del Monte; M. Feroci; M. Marisaldi
  ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES, Volume：207, Number：2, Aug. 2013, [Reviewed]
  We present Interplanetary Network (IPN) data for the gamma-ray bursts in the first Fermi Gamma-Ray Burst Monitor (GBM) catalog. Of the 491 bursts in that catalog, covering 2008 July 12 to 2010 July 11, 427 were observed by at least one other instrument in the nine-spacecraft IPN. Of the 427, the localizations of 149 could be improved by arrival time analysis (or "triangulation"). For any given burst observed by the GBM and one other distant spacecraft, triangulation gives an annulus of possible arrival directions whose half-width varies between about 0.'4 and 32 degrees, depending on the intensity, time history, and arrival direction of the burst, as well as the distance between the spacecraft. We find that the IPN localizations intersect the 1 sigma GBM error circles in only 52% of the cases, if no systematic uncertainty is assumed for the latter. If a 6 degrees systematic uncertainty is assumed and added in quadrature, the two localization samples agree about 87% of the time, as would be expected. If we then multiply the resulting error radii by a factor of three, the two samples agree in slightly over 98% of the cases, providing a good estimate of the GBM 3 sigma error radius. The IPN 3 sigma error boxes have areas between about 1 arcmin(2) and 110 deg(2), and are, on the average, a factor of 180 smaller than the corresponding GBM localizations. We identify two bursts in the IPN/GBM sample that did not appear in the GBM catalog. In one case, the GBM triggered on a terrestrial gamma flash, and in the other, its origin was given as "uncertain." We also discuss the sensitivity and calibration of the IPN.
  IOP PUBLISHING LTD, English, Scientific journal
  DOI：https://doi.org/10.1088/0067-0049/207/2/39
  DOI ID：10.1088/0067-0049/207/2/39, ISSN：0067-0049, eISSN：1538-4365, Web of Science ID：WOS:000322710000021
• Search for Non-Thermal Emissions from an Isolated Magnetic White Dwarf, EUVE J0317-855, with Suzaku　　　　　　　　　　　　　　　
  Atsushi Harayama; Yukikatsu Terada; Manabu Ishida; Takayuki Hayashi; Aya Bamba; Makoto S. Tashiro
  PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN, Volume：65, Number：4, Aug. 2013, [Reviewed]
  To search for possible non-thermal emissions from magnetic white dwarfs (WDs), we selected the most suitable candidates from among magnetic cataclysmic variables and isolated WDs. After the magnetic cataclysmic variable AE Aquarii, which emits hard X-ray pulses, the isolated WD EUVE J0317-855 is expected to emit the second most powerful magnetic dipole radiation with energies reaching similar to 1.1 x 10(29) erg s(-1). EUVE J0317-855 was observed with Suzaku from 2009 July 16 to 2009 July 17 for about 60 ks. No significant emissions were detected from the object in the 0.5-10 keV band, and the upper limit of the X-ray flux was estimated to be 1.7 x 10(-13) erg cm(-2) s(-1) in the 2-10 keV band. This value corresponds to less than 0.05% of the calculated spin-down energy. It excludes the possibility of explaining soft gamma-ray repeaters and anomalous X-ray pulsars as WDs, but may indicate that the activity in the magnetosphere of WDs is not so different from that occurring in radio pulsars. Curvature radiation, which is one of the suggested mechanism for emissions from the magnetosphere of compact objects, may explain the observed X-ray flux of AE Aquarii, and is consistent with the non-detection of EUVE J0317-855.
  OXFORD UNIV PRESS, English, Scientific journal
  DOI：https://doi.org/10.1093/pasj/65.4.73
  DOI ID：10.1093/pasj/65.4.73, ISSN：0004-6264, eISSN：2053-051X, Web of Science ID：WOS:000330328300004
• The interplanetary network　　　　　　　　　　　　　　　
  K. Hurley; I. G. Mitrofanov; D. Golovin; M. L. Litvak; A. B. Sanin; W. Boynton; C. Fellows; K. Harshman; R. Starr; S. Golenetskii; R. Aptekar; E. Mazets; V. Pal'Shin; D. Frederiks; D. Svinkin; D. M. Smith; W. Hajdas; A. Von Kienlin; X. Zhang; A. Rau; K. Yamaoka; T. Takahashi; M. Ohno; Y. Hanabata; Y. Fukazawa; M. Tashiro; Y. Terada; T. Murakami; K. Makishima; T. Cline; S. Barthelmy; J. Cummings; N. Gehrels; H. Krimm; D. Palmer; J. Goldsten; E. Del Monte; M. Feroci; M. Marisaldi; V. Connaughton; M. S. Briggs; C. Meegan
  EAS Publications Series, Volume：61, First page：459, Last page：464, 2013
  We describe the current, 9-spacecraft Interplanetary Network (IPN). The IPN detects about 325 gamma-ray bursts per year, of which about 100 are not localized by any other missions. We give some examples of how the data, which are public, can be utilized. © EAS, EDP Sciences 2013.
  English, International conference proceedings
  DOI：https://doi.org/10.1051/eas/1361074
  DOI ID：10.1051/eas/1361074, ISSN：1633-4760, SCOPUS ID：84887103930
• ORIGIN: metal creation and evolution from the cosmic dawn　　　　　　　　　　　　　　　
  Jan-Willem den Herder; Luigi Piro; Takaya Ohashi; Chryssa Kouveliotou; Dieter H. Hartmann; Jelle S. Kaastra; L. Amati; M. I. Andersen; M. Arnaud; J. -L. Atteia; S. Bandler; M. Barbera; X. Barcons; S. Barthelmy; S. Basa; S. Basso; M. Boer; E. Branchini; G. Branduardi-Raymont; S. Borgani; A. Boyarsky; G. Brunetti; C. Budtz-Jorgensen; D. Burrows; N. Butler; S. Campana; E. Caroli; M. Ceballos; F. Christensen; E. Churazov; A. Comastri; L. Colasanti; R. Cole; R. Content; A. Corsi; E. Costantini; P. Conconi; G. Cusumano; J. de Plaa; A. De Rosa; M. Del Santo; S. Di Cosimo; M. De Pasquale; R. Doriese; S. Ettori; P. Evans; Y. Ezoe; L. Ferrari; H. Finger; T. Figueroa-Feliciano; P. Friedrich; R. Fujimoto; A. Furuzawa; J. Fynbo; F. Gatti; M. Galeazzi; N. Gehrels; B. Gendre; G. Ghirlanda; G. Ghisellini; M. Gilfanov; P. Giommi; M. Girardi; J. Grindlay; M. Cocchi; O. Godet; M. Guedel; F. Haardt; R. den Hartog; I. Hepburn; W. Hermsen; J. Hjorth; H. Hoekstra; A. Holland; A. Hornstrup; A. van der Horst; A. Hoshino; J. in't Zand; K. Irwin; Y. Ishisaki; P. Jonker; T. Kitayama; H. Kawahara; N. Kawai; R. Kelley; C. Kilbourne; P. de Korte; A. Kusenko; I. Kuvvetli; M. Labanti; C. Macculi; R. Maiolino; M. Mas Hesse; K. Matsushita; P. Mazzotta; D. McCammon; M. Mendez; R. Mignani; T. Mineo; K. Mitsuda; R. Mushotzky; S. Molendi; L. Moscardini; L. Natalucci; F. Nicastro; P. O'Brien; J. Osborne; F. Paerels; M. Page; S. Paltani; K. Pedersen; E. Perinati; T. Ponman; E. Pointecouteau; P. Predehl; S. Porter; A. Rasmussen; G. Rauw; H. Rottgering; M. Roncarelli; P. Rosati; E. Quadrini; O. Ruchayskiy; R. Salvaterra; S. Sasaki; K. Sato; S. Savaglio; J. Schaye; S. Sciortino; M. Shaposhnikov; R. Sharples; K. Shinozaki; D. Spiga; R. Sunyaev; Y. Suto; Y. Takei; N. Tanvir; M. Tashiro; T. Tamura; Y. Tawara; E. Troja; M. Tsujimoto; T. Tsuru; P. Ubertini; J. Ullom; E. Ursino; F. Verbunt; F. van de Voort; M. Viel; S. Wachter; D. Watson; M. Weisskopf; N. Werner; N. White; R. Willingale; R. Wijers; N. Yamasaki; K. Yoshikawa; S. Zane
  EXPERIMENTAL ASTRONOMY, Volume：34, Number：2, First page：519, Last page：549, Oct. 2012
  ORIGIN is a proposal for the M3 mission call of ESA aimed at the study of metal creation from the epoch of cosmic dawn. Using high-spectral resolution in the soft X-ray band, ORIGIN will be able to identify the physical conditions of all abundant elements between C and Ni to red-shifts of z = 10, and beyond. The mission will answer questions such as: When were the first metals created? How does the cosmic metal content evolve? Where do most of the metals reside in the Universe? What is the role of metals in structure formation and evolution? To reach out to the early Universe ORIGIN will use Gamma-Ray Bursts (GRBs) to study their local environments in their host galaxies. This requires the capability to slew the satellite in less than a minute to the GRB location. By studying the chemical composition and properties of clusters of galaxies we can extend the range of exploration to lower redshifts (z similar to 0.2). For this task we need a high-resolution spectral imaging instrument with a large field of view. Using the same instrument, we can also study the so far only partially detected baryons in the Warm-Hot Intergalactic Medium (WHIM). The less dense part of the WHIM will be studied using absorption lines at low redshift in the spectra for GRBs. The ORIGIN mission includes a Transient Event Detector (coded mask with a sensitivity of 0.4 photon/cm(2)/s in 10 s in the 5-150 keV band) to identify and localize 2000 GRBs over a five year mission, of which similar to 65 GRBs have a redshift > 7. The Cryogenic Imaging Spectrometer, with a spectral resolution of 2.5 eV, a field of view of 30 arcmin and large effective area below 1 keV has the sensitivity to study clusters up to a significant fraction of the virial radius and to map the denser parts of the WHIM (factor 30 higher than achievable with current instruments). The payload is complemented by a Burst InfraRed Telescope to enable onboard red-shift determination of GRBs (hence securing proper follow up of high-z bursts) and also probes the mildly ionized state of the gas. Fast repointing is achieved by a dedicated Controlled Momentum Gyro and a low background is achieved by the selected low Earth orbit.
  SPRINGER, English, Scientific journal
  DOI：https://doi.org/10.1007/s10686-011-9224-7
  DOI ID：10.1007/s10686-011-9224-7, ISSN：0922-6435, eISSN：1572-9508, Web of Science ID：WOS:000309230600014
• INVERSE COMPTON X-RAY EMISSION FROM SUPERNOVAE WITH COMPACT PROGENITORS: APPLICATION TO SN2011fe　　　　　　　　　　　　　　　
  R. Margutti; A. M. Soderberg; L. Chomiuk; R. Chevalier; K. Hurley; D. Milisavljevic; R. J. Foley; J. P. Hughes; P. Slane; C. Fransson; M. Moe; S. Barthelmy; W. Boynton; M. Briggs; V. Connaughton; E. Costa; J. Cummings; E. Del Monte; H. Enos; C. Fellows; M. Feroci; Y. Fukazawa; N. Gehrels; J. Goldsten; D. Golovin; Y. Hanabata; K. Harshman; H. Krimm; M. L. Litvak; K. Makishima; M. Marisaldi; I. G. Mitrofanov; T. Murakami; M. Ohno; D. M. Palmer; A. B. Sanin; R. Starr; D. Svinkin; T. Takahashi; M. Tashiro; Y. Terada; K. Yamaoka
  ASTROPHYSICAL JOURNAL, Volume：751, Number：2, Jun. 2012, [Reviewed]
  We present a generalized analytic formalism for the inverse Compton X-ray emission from hydrogen-poor supernovae and apply this framework to SN 2011fe using Swift X-Ray Telescope (XRT), UVOT, and Chandra observations. We characterize the optical properties of SN 2011fe in the Swift bands and find them to be broadly consistent with a "normal" SN Ia, however, no X-ray source is detected by either XRT or Chandra. We constrain the progenitor system mass-loss rate (M) over dot < 2 x 10(-9) M-circle dot yr(-1) (3 sigma c.l.) for wind velocity v(w) = 100 km s(-1). Our result rules out symbiotic binary progenitors for SN 2011fe and argues against Roche lobe overflowing subgiants and main-sequence secondary stars if greater than or similar to 1% of the transferred mass is lost at the Lagrangian points. Regardless of the density profile, the X-ray non-detections are suggestive of a clean environment (n(CSM) < 150 cm(-3)) for 2 x 10(15) less than or similar to R less than or similar to 5 x 10(16) cm around the progenitor site. This is either consistent with the bulk of material being confined within the binary system or with a significant delay between mass loss and supernova explosion. We furthermore combine X-ray and radio limits from Chomiuk et al. to constrain the post-shock energy density in magnetic fields. Finally, we searched for the shock breakout pulse using gamma-ray observations from the Interplanetary Network and find no compelling evidence for a supernova-associated burst. Based on the compact radius of the progenitor star we estimate that the shock breakout pulse was likely not detectable by current satellites.
  IOP PUBLISHING LTD, English, Scientific journal
  DOI：https://doi.org/10.1088/0004-637X/751/2/134
  DOI ID：10.1088/0004-637X/751/2/134, ISSN：0004-637X, Web of Science ID：WOS:000304204600055
• The High-Resolution X-Ray Microcalorimeter Spectrometer, SXS, on Astro-H　　　　　　　　　　　　　　　
  Mitsuda Kazuhisa; Kelley Richard L; Boyce Kevin R; Brown Gregory V; Costantini Elisa; DiPirro Michael J; Ezoe Yuichiro; Fujimoto Ryuichi; Gendreau Keith C; den Herder Jan-Willem; Hoshino Akio; Ishisaki Yoshitaka; Kilbourne Caroline A; Kitamoto Shunji; McCammon Dan; Murakami Masahide; Murakami Hiroshi; Ogawa Mina; Ohashi Takaya; Okamoto Atsushi; Paltani Stephane; Pohl Martin; Porter F. Scott; Sato Yoichi; Shinozaki Keisuke; Shirron Peter J; Sneiderman Gary A; Sugita Hiroyuki; Szymkowiak Andrew; Takei Yoh; Tamagawa Toru; Tashiro Makoto; Terada Yukikatsu; Tsujimoto Masahiro; de Vries Cor; Yamasaki Noriko Y
  JOURNAL OF LOW TEMPERATURE PHYSICS, Volume：167, Number：5-6, First page：795, Last page：802, Jun. 2012, [Reviewed]
  DOI：https://doi.org/10.1007/s10909-012-0482-1
  DOI ID：10.1007/s10909-012-0482-1, ISSN：0022-2291, Web of Science ID：WOS:000303461600036
• Hard X-ray properties of a variable standard candle, Crab, with the Suzaku/HXD
  Kouzu, T; Terada, Y; Tashiro, M.S; Yamada, S; Bamba, A; Yuasa, T; Mori, K; Fukazawa, Y; Enoto, T; Tanaka, Y.T; Shibata, S; Makishima, K
  AIP Conference Proceedings, Volume：1427, First page：265, Last page：266, May 2012
  The Crab Nebula had been believed to be a stable standard candle for historical X-ray instruments for many years. Recently it was found that a hard X-ray flux (15-100 keV) of Crab Nebula fluctuated by 10 over 10 years. The origin of the long-term variation is still unclear, but the nature of the Crab Nebula is now hot topic both on science and hardware developments. The HXD onboard Suzaku has the highest sensitivity in the 10-600 keV band. Hence it is useful to search for flux variations and possible spectral changes. We performed systematic studies on Crab X-ray spectra in the 10-600 keV band w ith the HXD, by using 12 observations of Crab until 2010. In this paper, we summarized a hard X-ray study of Crab with the HXD. © 2012 American Institute of Physics.
  AIP Conference Proceedings, English, International conference proceedings
  DOI：https://doi.org/10.1063/1.3696196
  DOI ID：10.1063/1.3696196
• POSSIBLE DETECTION OF AN EMISSION CYCLOTRON RESONANCE SCATTERING FEATURE FROM THE ACCRETION-POWERED PULSAR 4U 1626-67　　　　　　　　　　　　　　　
  W. B. Iwakiri; Y. Terada; T. Mihara; L. Angelini; M. S. Tashiro; T. Enoto; S. Yamada; K. Makishima; M. Nakajima; A. Yoshida
  ASTROPHYSICAL JOURNAL, Volume：751, Number：1, First page：35, May 2012, [Reviewed]
  We present analysis of 4U 1626-67, a 7.7 s pulsar in a low-mass X-ray binary system, observed with the hard X-ray detector of the Japanese X-ray satellite Suzaku in 2006 March for a net exposure of similar to 88 ks. The source was detected at an average 10-60 keV flux of similar to 4 x 10(-10) erg cm(-2) s(-1). The phase-averaged spectrum is reproduced well by combining a negative and positive power-law times exponential cutoff (NPEX) model modified at similar to 37 keV by a cyclotron resonance scattering feature (CRSF). The phase-resolved analysis shows that the spectra at the bright phases are well fit by the NPEX with CRSF model. On the other hand, the spectrum in the dim phase lacks the NPEX high-energy cutoff component, and the CRSF can be reproduced by either an emission or an absorption profile. When fitting the dim phase spectrum with the NPEX plus Gaussian model, we find that the feature is better described in terms of an emission rather than an absorption profile. The statistical significance of this result, evaluated by means of an F test, is between 2.91 x 10(-3) and 1.53 x 10(-5), taking into account the systematic errors in the background evaluation of HXD-PIN. We find that the emission profile is more feasible than the absorption one for comparing the physical parameters in other phases. Therefore, we have possibly detected an emission line at the cyclotron resonance energy in the dim phase.
  IOP PUBLISHING LTD, English, Scientific journal
  DOI：https://doi.org/10.1088/0004-637X/751/1/35
  DOI ID：10.1088/0004-637X/751/1/35, ISSN：0004-637X, eISSN：1538-4357, Web of Science ID：WOS:000303814600035
• Spectral Evolutions in Gamma-Ray Burst Exponential Decays Observed with Suzaku WAM　　　　　　　　　　　　　　　
  Makoto S. Tashiro; Kaori Onda; Kazutaka Yamaoka; Masahiro Ohno; Satoshi Sugita; Takeshi Uehara; Hiromi Seta
  PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN, Volume：64, Number：2, Apr. 2012, [Reviewed]
  This paper presents a study on the spectral evolution of gamma-ray burst (GRB) prompt emissions observed with the Suzaku Wide-band All-sky Monitor (WAM). By making use of the WAM data archive, 6 bright GRBs exhibiting 7 well-separated fast-rise-exponential-decay (FRED) shaped light curves are presented, and the evaluated exponential decay time constants of the energy-resolved light curves from these FRED peak light curves are shown to indicate significant spectral evolution. The energy dependence of the time constants is well described with a power-law function, tau(E) alpha E-gamma, where gamma similar to -(0.34 +/- 0.12) on average, although 5 FRED peaks show a consistent value of gamma = -1/2, which is expected in synchrotron or inverse-Compton cooling models. In particular, 2 of the GRBs were located with accuracy sufficient to evaluate the time-resolved spectra with precise energy response matrices. Their behavior in spectral evolution suggests two different origins of emissions. In the case of GRB 081224, the derived 1-s time-resolved spectra are well described by a blackbody radiation model with a power-law component. The derived behavior of cooling is consistent with that expected from radiative cooling or expansion of the emission region. On the other hand, the other 1-s time-resolved spectra from GRB 100707A is well described by a Band GRB model as well as with the thermal model. Although relative poor statistics prevent us to conclude, the energy dependence in the decaying light curve is consistent with that expected in the former emission mechanism model.
  OXFORD UNIV PRESS, English, Scientific journal
  DOI：https://doi.org/10.1093/pasj/64.2.26
  DOI ID：10.1093/pasj/64.2.26, ISSN：0004-6264, eISSN：2053-051X, Web of Science ID：WOS:000304028200006
• ENERGETIC FERMI/LAT GRB 100414A: ENERGETIC AND CORRELATIONS　　　　　　　　　　　　　　　
  Yuji Urata; Kuiyun Huang; Kazutaka Yamaoka; Patrick P. Tsai; Makoto S. Tashiro
  ASTROPHYSICAL JOURNAL LETTERS, Volume：748, Number：1, Mar. 2012, [Reviewed]
  This study presents multi-wavelength observational results for energetic GRB 100414A with GeV photons. The prompt spectral fitting using Suzaku/WAM data yielded spectral peak energies of E-peak(src) of 1458.7(-106.6)(+132.6) keV and E-iso of 34.5(-1.8)(+2.0) x 10(52) erg with z = 1.368. The optical afterglow light curves between 3 and 7 days were effectively fitted according to a simple power law with a temporal index of alpha = -2.6 +/- 0.1. The joint light curve with earlier Swift/UVOT observations yields a temporal break at 2.3 +/- 0.2 days. This was the first Fermi/LAT detected event that demonstrated the clear temporal break in the optical afterglow. The jet opening angle derived from this temporal break was 5 degrees.8, consistent with those of other well-observed long gamma-ray bursts (GRBs). The multi-wavelength analyses in this study showed that GRB 100414A follows E-peak(src)-E-iso and E-peak(src)-E-gamma correlations. The late afterglow revealed a flatter evolution with significant excesses at 27.2 days. The most straightforward explanation for the excess is that GRB 100414A was accompanied by a contemporaneous supernova. The model light curve based on other GRB-SN events is marginally consistent with that of the observed light curve.
  IOP PUBLISHING LTD, English, Scientific journal
  DOI：https://doi.org/10.1088/2041-8205/748/1/L4
  DOI ID：10.1088/2041-8205/748/1/L4, ISSN：2041-8205, eISSN：2041-8213, Web of Science ID：WOS:000301297500004
• A spectral study of the black hole candidate XTE J1752-223 in the high/soft state with MAXI, Suzaku, and Swift　　　　　　　　　　　　　　　
  Satoshi Nakahira; Shu Koyama; Yoshihiro Ueda; Kazutaka Yamaoka; Mutsumi Sugizaki; Tatehiro Mihara; Masaru Matsuoka; Atsumasa Yoshida; Kazuo Makishima; Ken Ebisawa; Aya Kubota; Shin'ya Yamada; Hitoshi Negoro; Kazuo Hiroi; Masaki Ishikawa; Nobuyuki Kawai; Masashi Kimura; Hiroki Kitayama; Mitsuhiro Kohama; Takanori Matsumura; Mikio Morii; Motoki Nakajima; Motoko Serino; Megumi Shidatsu; Tetsuya Sootome; Kousuke Sugimori; Fumitoshi Suwa; Hiroshi Tomida; Yoko Tsuboi; Hiroshi Tsunemi; Shiro Ueno; Ryuichi Usui; Takayuki Yamamoto; Kyohei Yamazaki; Makoto S. Tashiro; Yukikatsu Terada; Hiromi Seta
  Publications of the Astronomical Society of Japan, Volume：64, Number：1, Feb. 2012, [Reviewed]
  We report on an X-ray spectral analysis of the black hole candidate XTE J1752-223 in the 2009-2010 outburst, utilizing data obtained with the MAXI/Gas Slit Camera (GSC), the Swift/XRT, and Suzaku, which work comple-mentarily. As already reported by Nakahira et al. (2010, PASJ, 62, L27), MAXI monitored the source continuously throughout the entire outburst for about eight months. All of the MAXI/GSC energy spectra in the high/soft state, lasting for 2 months, are well represented by a multi-color disk plus power-law model. The innermost disk temperature changed from ∼0.7 keV to ∼0.4 keV and the disk flux decreased by an order of magnitude. Nevertheless, the innermost radius is constant at ∼41 D 3.5 (cos i) -1/2 km, where D 3.5 is the source distance in units of 3.5kpc and i the inclination. The multi-color disk parameters obtained with the MAXI/GSC are consistent with those with the Swift/XRT and Suzaku. The Suzaku data also suggest a possibility that the disk emission is slightly Comptonized, which could account for broad iron-K features reported previously. Assuming that the obtained innermost radius represents the innermost stable circular orbit for a non-rotating black hole, we estimate the mass of the black hole to be 5.51 ± 0.28 M ⊙ D 3.5 (cos -1/2 , where the correction for the stress-free inner boundary condition and color hardening factor of 1.7 are taken into account. If the inclination is less than 49°, as suggested from radio monitoring of transient jets, and the soft-to-hard transition in 2010 April occurred at 1%-4% of Eddignton luminosity, the fitting of the Suzaku spectra with a relativistic accretion-disk model derives constraints on the mass and the distance to be 3.1-55M ⊙ and 2.3-22 kpc, respectively. This confirms that the compact object in XTE J1752-223 is a black hole. © 2012. Astronomical Society of Japan.
  Scientific journal
  DOI：https://doi.org/10.1093/pasj/64.1.13
  Scopus：https://www.scopus.com/inward/record.uri?partnerID=HzOxMe3b&scp=84863287542&origin=inward
  Scopus Citedby：https://www.scopus.com/inward/citedby.uri?partnerID=HzOxMe3b&scp=84863287542&origin=inward
  DOI ID：10.1093/pasj/64.1.13, ISSN：0004-6264, SCOPUS ID：84863287542, Web of Science ID：WOS:000301307500013
• The interplanetary network database　　　　　　　　　　　　　　　
  K. Hurley; I. G. Mitrofanov; D. Golovin; M. L. Litvak; A. B. Sanin; W. Boynton; C. Fellows; K. Harshman; R. Starr; S. Golenetskii; R. Aptekar; E. Mazets; V. Pal'shin; D. Frederiks; D. Svinkin; D. M. Smith; W. Hajdas; A. Von Kienlin; X. Zhang; A. Rau; K. Yamaoka; T. Takahashi; M. Ohno; Y. Hanabata; Y. Fukazawa; M. Tashiro; Y. Terada; T. Murakami; K. Makishima; T. Cline; S. Barthelmy; J. Cummings; N. Gehrels; H. Krimm; D. Palmer; J. Goldsten; E. Del Monte; M. Feroci; M. Marisaldi; V. Connaughton; M. S. Briggs; C. Meegan
  Proceedings of Science, Volume：2012-, 2012
  Interplanetary Networks (IPNs) have been in use since the late 1970’s. The current IPN comprises 9 spacecraft and detects about 325 GRBs/year, roughly 100 of which are not localized by Swift or Fermi. It is an all-sky, full-time monitor for short-duration gamma-ray transients. We describe the IPN database, which is publicly available on the IPN website. It comprises, among other things, a GRB bibliography, a comprehensive list of bursts from 1990 to the present, and localization data. We also describe some of the uses of the IPN data.
  Sissa Medialab Srl, English, International conference proceedings
  ISSN：1824-8039, SCOPUS ID：85052382495
• Energetic Fermi/LAT GRB100414A: Energetic and correlations　　　　　　　　　　　　　　　
  Yuji Urata; Kuiyun Huang; Kazutaka Yamaoka; Makoto S. Tashiro
  Proceedings of Science, Volume：2012-, 2012
  We present multi-wavelength observational results for energetic GRB 100414A with GeV photons. The prompt spectral fitting using Suzaku/WAM data yielded the spectral peak energies of Epeak src of 1458.7+ − 132 106 6 6 keV and Eiso of 34.5− + 1 2 8 0 × 1052 erg with z = 1.368. The optical afterglow light curves between 3 and 7 days were well fitted by a simple power law with a temporal index of α = −2.6 ± 0.1. The joint light curve with earlier Swift/UVOT observations yields a temporal break at 2.3±0.2 days. This was the first Fermi/LAT detected event that demonstrated the clear temporal break in the optical afterglow. The jet opening angle derived from this temporal break was ∼ 5.8◦, consistent with those of other well-observed long GRBs. Our multi-wavelength analyses showed that GRB 100414A follows Epeak src − Eiso and Epeak src − Eγ correlations. The late afterglow revealed a flatter evolution with the significant excesses at 27.2 days. The most straightforward explanation for the excess is that GRB 100414A was accompanied by a contemporaneous supernova. The model light curve based on other GRB-SNe events is marginally consistent with the observed one.
  Sissa Medialab Srl, English, International conference proceedings
  ISSN：1824-8039, SCOPUS ID：85052369846
• First X-ray Detection from a Bow Shock Region of a Runaway Star, BD+43 degrees 3654, with Suzaku　　　　　　　　　　　　　　　
  Y. Terada; M. S. Tashiro; A. Bamba; R. Yamazaki; H. Seta; T. Kouzu; S. Koyama
  SUZAKU 2011: EXPLORING THE X-RAY UNIVERSE: SUZAKU AND BEYOND, Volume：1427, 2012, [Reviewed]
  Searching for new types of particle-acceleration sites is important. Recently, Synchrotron emission has been reported from a bow shock region from a runway star BD+43 degrees 3654 with a radio observation by VLA. It was the first discovery of a non-thermal emission from a runaway star. In order to search for possible non-thermal tail in the X-ray band, we have performed the observation of the object BD+43 degrees 3654 with Suzaku in April 2011 with the exposure of 105 ksec. As a result, thanks to the stable low-background capability of the XIS, we detected X-rays around the bow shock region. The X-ray luminosity of the diffuse X-rays around the object was about 10(31) erg s(-1) in the 0.5 to 10 keV band. In addition, we also detected X-rays from the object itself, BD+43 degrees 3654, representing a thermal X-ray spectrum with a temperature of 0.6 keV at the luminosity of 1.3x10(31) erg s(-1) in the same band. Detail analyses will be reported in a future paper. The results suggest the conversion efficiency from the momentum of the stellar wind into accelerated electrons would be the same order of magnitudes of those seen in shocks of supernova remnants.
  AMER INST PHYSICS, English, International conference proceedings
  DOI：https://doi.org/10.1063/1.3696151
  DOI ID：10.1063/1.3696151, ISSN：0094-243X, Web of Science ID：WOS:000302776900009
• Soft Gamma-ray Detector for the ASTRO-H mission　　　　　　　　　　　　　　　
  Shin Watanabe; Hiroyasu Talima; Yasushi Fukazawa; Roger Blandford; Teruaki Enoto; Jun Kataoka; Madoka Kawaharada; Motohide Kokubun; Philippe Laurent; Francois Lebrun; Olivier Limousin; Greg Madejski; Kazuo Makishima; Tsunefumi Mizuno; Takeshi Nakamori; Kazuhiro Nakazawa; Kunishiro Mori; Hirokazu Odaka; Masanori Ohno; Masayuki Ohta; Goro Sato; Rie Sato; Shin'ichiro Takeda; Hiromitsu Takahashi; Tadayuki Takahashi; Takaaki Tanaka; Makoto Tashiro; Yukikatsu Terada; Hideki Uchiyama; Yasunobu Uchiyama; Shinya Yamada; Yoichi Yatsu; Daisuke Yonetoku; Takayuki Yuasa
  SPACE TELESCOPES AND INSTRUMENTATION 2012: ULTRAVIOLET TO GAMMA RAY, Volume：8443, First page：844326, Last page：19pp, 2012
  ASTRO-H is the next generation JAXA X-ray satellite, intended to carry instruments with broad energy coverage and exquisite energy resolution. The Soft Gamma-ray Detector (SGD) is one of ASTRO-H instruments and will feature wide energy band (60-600 keV) at a background level 10 times better than the current instruments on orbit. The SGD is complimentary to ASTRO-H's Hard X-ray Imager covering the energy range of 5-80 keV. The SGD achieves low background by combining a Compton camera scheme with a narrow field-of-view active shield where Compton kinematics is utilized to reject backgrounds. The Compton camera in the SGD is realized as a hybrid semiconductor detector system which consists of silicon and CdTe (cadmium telluride) sensors. Good energy resolution is afforded by semiconductor sensors, and it results in good background rejection capability due to better constraints on Compton kinematics. Utilization of Compton kinematics also makes the SGD sensitive to the gamma-ray polarization, opening up a new window to study properties of gamma-ray emission processes. In this paper, we will present the detailed design of the SGD and the results of the final prototype developments and evaluations. Moreover, we will also present expected performance based on the measurements with prototypes.
  SPIE-INT SOC OPTICAL ENGINEERING, English, International conference proceedings
  DOI：https://doi.org/10.1117/12.925977
  DOI ID：10.1117/12.925977, ISSN：0277-786X, eISSN：1996-756X, Web of Science ID：WOS:000312391600059
• The time assignment system of ASTRO-H　　　　　　　　　　　　　　　
  Tomomi Kouzu; Kaori Iwase; Yuki Mishima; Yukikatsu Terada; Takayuki Yuasa; Yoshitaka Ishisaki; Makoto S. Tashiro; Motohide Kokubun; Masanobu Ozaki; Masaharu Nomachi; Tadayuki Takahashi
  IEEE Nuclear Science Symposium Conference Record, First page：163, Last page：166, 2012, [Reviewed]
  ASTRO-H is an X-ray astronomy satellite to be launched in 2014. The data acquisition system of this mission is realized with a standard network protocol, SpaceWire. Although the protocol itself is well designed, a new concept to grantee the quality of service will be installed to the ASTRO-H data acquisition system. Therefore, the verification of the design of the concept is essential in the initial phase of the development. The time assignment function is one of the important issues for the SpaceWire development. The accuracy of the absolute time of about 30 μs is required from science goals. The key point of the time assignment with SpaceWire network in the ASTRO-H system is how accurately sharing the time information. In this paper, our design of the time distribution and assignment system for ASTRO-H is shown. The results of our measurements of timing accuracy are also presented to show that the design will fulfill the goal of absolute timing accuracy. © 2011 IEEE.
  English, International conference proceedings
  DOI：https://doi.org/10.1109/NSSMIC.2011.6154471
  DOI ID：10.1109/NSSMIC.2011.6154471, ISSN：1095-7863, SCOPUS ID：84863348846
• Evolution of the jet energetics revealed with the Suzaku observations of giant radio galaxies　　　　　　　　　　　　　　　
  Naoki Isobe; Hiromi Seta; Makoto S. Tashiro; Gandhi Poshak; Matsuta Keiko
  SUZAKU 2011: EXPLORING THE X-RAY UNIVERSE: SUZAKU AND BEYOND, Volume：1427, 2012, [Reviewed]
  Suzaku observations are reported of the three giant radio galaxies, 3C 35, 3C 326, and DA 240, with a projected linear size of greater than or similar to 1 Mpc. The low and stable instrumental background of the X-ray Imaging Spectrometer onboard Suzaku allows a significant detection of inverse Compton X-ray emission from the lobes of these giant radio galaxies. As a result, the electron and magnetic energy densities in the lobes were measured. Based on the measurements, the late phase in the evolution of the energetics associated with jets from active galactic nuclei was investigated. It is found that the lobes of giant radio galaxies tend to reside in a near equipartition condition between electrons and magnetic field, despite the fact that smaller sources with sizes of about 100 kpc exhibit a particle dominance by a typical factor of 10 in energy density. In addition, the energy densities in the giant lobes are measured to be smaller by an order of magnitude as compared to the extrapolation of the size to energy density correlation found for smaller radio galaxies. These results indicate that typical radio galaxies experience a significant reduction in their jet power, as their jets evolve in size from 100 kpc to 1 Mpc.
  AMER INST PHYSICS, English, International conference proceedings
  DOI：https://doi.org/10.1063/1.3696174
  DOI ID：10.1063/1.3696174, ISSN：0094-243X, Web of Science ID：WOS:000302776900032
• The Suzaku HXD-WAM in the 3rd Interplanetary Network - A Cycle 1-5 Guest Investigator Project　　　　　　　　　　　　　　　
  K. Hurley; K. Yamaoka; Y. Fukazawa; Y. Hanabata; T. Murakami; T. Takahashi; M. Ohno; M. Tashiro; Y. Terada
  SUZAKU 2011: EXPLORING THE X-RAY UNIVERSE: SUZAKU AND BEYOND, Volume：1427, 2012, [Reviewed]
  The BGO anticoincidence shield of the Suzaku Hard X-Ray Detector Wideband All-Sky Monitor (HXD WAM) has been designed to act as a gamma-ray burst detector. It was incorporated into the 3rd interplanetary network shortly after launch, and it is now detecting about one confirmed gamma-ray or soft gamma repeater burst every 2.5 days. It has detected almost 900 events so far.
  AMER INST PHYSICS, English, International conference proceedings
  DOI：https://doi.org/10.1063/1.3696236
  DOI ID：10.1063/1.3696236, ISSN：0094-243X, Web of Science ID：WOS:000302776900094
• Spectral Evolutions Study of Gamma-Ray Burst Exponential Decays with Suzaku-WAM　　　　　　　　　　　　　　　
  Makoto S. Tashiro; Kaori Onda; Kazutaka Yamaoka; Masahiro Ohno; Satoshi Sugita; Takeshi Uehara; Hiromi Seta
  DEATH OF MASSIVE STARS: SUPERNOVAE AND GAMMA-RAY BURSTS, Number：279, First page：411, Last page：412, 2012, [Reviewed]
  An observational study is presented of the spectral evolution of gamma-ray burst (GRB) prompt emissions with the Suzaku Wide-band All-sky Monitor (WAM). We selected 6 bright GRBs exhibiting 7 well-separated fast-rise-exponential-decay (FRED) shaped light curves to investigate spectral changes by evaluating exponential decay time constants of the energy resolved light curves. In addition, we carried out time-resolved spectroscopy of two of them which were located with accuracy sufficient to evaluate the time-resolved spectra with precise energy response matrices. The two imply different emission mechanisms; the one is well reproduced with a cooling blackbody radiation model with a power-law component, while the other prefers non-thermal emission model with a decaying turn over energy.
  CAMBRIDGE UNIV PRESS, English, International conference proceedings
  DOI：https://doi.org/10.1017/S1743921312013592
  DOI ID：10.1017/S1743921312013592, ISSN：1743-9213, Web of Science ID：WOS:000393362200099
• Concept of a small satellite for sub-MeV & MeV all sky survey: the CAST mission　　　　　　　　　　　　　　　
  Nakazawa, Kazuhiro; Takahashi, Tadayuki; Ichinohe, Yuto; Takeda, Shin'ichiro; Tajima, Hiroyasu; Kamae, Tuneyoshi; Kokubun, Motohide; Takashima, Takeshi; Tashiro, Makoto; Tamagawa, Toru; Terada, Yukikatsu; Nomachi, Masaharu; Fukazawa, Yasushi; Makishima, Kazuo; Mizuno, Tsunefumi; Mitani, Takefumi; Yoshimitsu, Tetsuo; Watanabe, Shin
  SPACE TELESCOPES AND INSTRUMENTATION 2012: ULTRAVIOLET TO GAMMA RAY, Volume：8443, 2012, [Reviewed]
  MeV and sub-MeV energy band from similar to 200 keV to similar to 2 MeV contains rich information of high-energy phenomena in the universe. The CAST (Compton Telescope for Astro and Solar Terrestrial) mission is planned to be launched at the end of 2010s, and aims at providing all-sky map in this energy-band for the first time. It is made of a semiconductor Compton telescope utilizing Si as a scatterer and CdTe as an absorber. CAST provides all-sky sub-MeV polarization map for the first time, as well. The Compton telescope technology is based on the design used in the Soft Gamma-ray Detector (SGD) onboard ASTRO-H, characterized by its tightly stacked semiconductor layers to obtain high Compton reconstruction efficiency. The CAST mission is currently planned as a candidate for the small scientific satellite series in ISAS/JAXA, weighting about 500 kg in total. Scalable detector design enables us to consider other options as well. Scientific outcome of CAST is wide. It will provide new information from high-energy sources, such as AGN and/or its jets, supernova remnants, magnetors, black-hole and neutron-star binaries and others. Polarization map will tell us about activities of jets and reflections in these sources, as well. In addition, CAST will simultaneously observe the Sun, and depending on its attitude, the Earth.
  SPIE-INT SOC OPTICAL ENGINEERING, English, International conference proceedings
  DOI：https://doi.org/10.1117/12.926164
  DOI ID：10.1117/12.926164, ISSN：0277-786X, eISSN：1996-756X, Web of Science ID：WOS:000312391600011
• THE INTERPLANETARY NETWORK SUPPLEMENT TO THE HETE-2 GAMMA-RAY BURST CATALOG　　　　　　　　　　　　　　　
  K. Hurley; J. -L. Atteia; C. Barraud; A. Pelangeon; M. Boer; R. Vanderspek; G. Ricker; E. Mazets; S. Golenetskii; D. D. Frederiks; V. D. Pal'shin; R. L. Aptekar; D. M. Smith; C. Wigger; W. Hajdas; A. Rau; A. von Kienlin; I. G. Mitrofanov; D. V. Golovin; A. S. Kozyrev; M. L. Litvak; A. B. Sanin; W. Boynton; C. Fellows; K. Harshman; S. Barthelmy; T. Cline; J. Cummings; N. Gehrels; H. A. Krimm; K. Yamaoka; Y. Fukazawa; Y. Hanabata; M. Ohno; T. Takahashi; M. Tashiro; Y. Terada; T. Murakami; K. Makishima; C. Guidorzi; F. Frontera; C. E. Montanari; F. Rossi; J. Trombka; T. McClanahan; R. Starr; J. Goldsten; R. Gold
  ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES, Volume：197, Number：2, Dec. 2011, [Reviewed]
  Between 2000 November and 2006 May, one or more spacecraft of the interplanetary network (IPN) detected 226 cosmic gamma-ray bursts that were also detected by the French Gamma-Ray Telescope experiment on board the High Energy Transient Experiment 2 spacecraft. During this period, the IPN consisted of up to nine spacecraft, and using triangulation, the localizations of 157 bursts were obtained. We present the IPN localization data on these events.
  IOP PUBLISHING LTD, English, Scientific journal
  DOI：https://doi.org/10.1088/0067-0049/197/2/34
  DOI ID：10.1088/0067-0049/197/2/34, ISSN：0067-0049, eISSN：1538-4365, Web of Science ID：WOS:000298244300020
• Improvements in Calibration of GSO Scintillators in the Suzaku Hard X-Ray Detector　　　　　　　　　　　　　　　
  Yamada Shin'ya; Makishima Kazuo; Nakazawa Kazuhiro; Kokubun Motohide; Kawaharada Madoka; Kitaguchi Takao; Watanabe Shin; Takahashi Hiromitsu; Noda Hirofumi; Nishioka Hiroyuki; Hiragi Kazuyoshi; Hayashi Katsuhiro; Nakajima Kenta; Tashiro Makoto; Sasano Makoto; Nishino Sho; Torii Shunsuke; Sakurai Soki; Takahashi Tadayuki; Mizuno Tsunefumi; Enoto Teruaki; Yuasa Takayuki; Tanaka Takaaki; Kouzu Tomomi; Nakano Toshio; Fukazawa Yasushi; Terada Yukikatsu; Uchiyama Yasunobu; Iwakiri Wataru
  PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN, Volume：63, Number：SPEC. ISSUE 3, First page：S645, Last page：S656, Nov. 2011, [Reviewed]
  Improvements of the in-orbit calibration of GSO scintillators in the Hard X-ray Detector aboard Suzaku are reported. To resolve an apparent change in the energy scale of GSO, which appeared across the launch for unknown reasons, consistent and thorough re-analyses of both pre-launch and in-orbit data have been performed. With laboratory experiments using spare hardware, the pulse-height offset, corresponding to zero energy input, was found to change by ∼0.5% of the full analog voltage scale, depending on the power supply. Furthermore, by carefully calculating all of the light outputs of secondaries from activation lines used in the in-orbit gain determination, their energy deposits in GSO were found to be effectively lower, by several percent, than their nominal energies. Taking both of these effects into account, the in-orbit data agree with the on-ground measurements within ∼5%, without employing the artificial correction introduced in previous work (Kokubun et al. 2007, PASJ, 59, S53). With this knowledge, we updated the data processing, the response, and the auxiliary files of GSO, and reproduced the HXD-PIN and HXD-GSO spectra of the Crab Nebula over 12-300 keV by a broken power-law with a break energy of ∼110 keV. © 2011. Astronomical Society of Japan.
  Scientific journal
  DOI：https://doi.org/10.1093/pasj/63.sp3.S645
  Scopus：https://www.scopus.com/inward/record.uri?partnerID=HzOxMe3b&scp=82555200911&origin=inward
  Scopus Citedby：https://www.scopus.com/inward/citedby.uri?partnerID=HzOxMe3b&scp=82555200911&origin=inward
  DOI ID：10.1093/pasj/63.sp3.S645, ISSN：0004-6264, SCOPUS ID：82555200911, Web of Science ID：WOS:000299191800003
• Suzaku Measurement of Electron and Magnetic Energy Densities in the East Lobe of the Giant Radio Galaxy DA 240　　　　　　　　　　　　　　　
  Naoki Isobe; Hiromi Seta; Makoto S. Tashiro
  PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN, Volume：63, First page：S947, Last page：S955, Nov. 2011, [Reviewed]
  A careful analysis of the Suzaku data of the giant radio galaxy DA 240, of which the size is 1.48 Mpc, revealed diffuse X-ray emission associated with its east lobe. The diffuse X-ray spectrum was described with a simple power-law model with a photon index of Gamma = 1.92(-0.17-0.06)(+0.13+0.04) where the first and second errors represent the statistical and systematic ones. The agreement with the synchrotron radio photon index, Gamma(R) = 1.95 +/- 0.01 in 326-608.5 MHz, ensures that any excess X-ray emission is attributed to inverse Compton emission from the synchrotron-radiating electrons, boosting up the cosmic microwave background photons. From the X-ray flux density, 51.5 +/- 3.91(-5.4)(+6.2) nJy at 1 keV, derived with the photon index fixed at Gamma(R), in comparison with the synchrotron radio intensity of 10.30 +/- 0.12 Jy at 326 MHz, the magnetic and electron energy densities were estimated as u(m) = (3.0 +/- 0.2 +/- 0.4) x 10(-14)erg cm(-3) and u(e) =(34(-0.2-0.4)(+0.3+0.5)) x 10(-14)erg cm(-3) integrated over the electron Lorentz factor of 10(3)-10(5), respectively. Thus, the east lobe is found to reside in an equipartition condition between the electrons and magnetic field parametrized as u(e)/u(m) = 1.1(-0.1-0.2)(+0.2+0.4). The east lobe of DA 240 is indicated to exhibit the lowest value of tie, among all of the X-ray detected lobes of radio galaxies. A comparison of the energetics in the giant radio galaxies with a size of 1 Mpc to those in the smaller objects suggests a possibility that radio galaxies lose their jet power as they evolve from similar to 100 kpc to similar to 1 Mpc.
  OXFORD UNIV PRESS, English, Scientific journal
  DOI：https://doi.org/10.1093/pasj/63.sp3.S947
  DOI ID：10.1093/pasj/63.sp3.S947, ISSN：0004-6264, eISSN：2053-051X, Web of Science ID：WOS:000299191800032
• Search for gravitational wave bursts from six magnetars　　　　　　　　　　　　　　　
  J. Abadie; B. P. Abbott; R. Abbott; M. Abernathy; T. Accadia; F. Acernese; C. Adams; R. Adhikari; C. Affeldt; B. Allen; G. S. Allen; E. Amador Ceron; D. Amariutei; R. S. Amin; S. B. Anderson; W. G. Anderson; F. Antonucci; K. Arai; M. A. Arain; M. C. Araya; S. M. Aston; P. Astone; D. Atkinson; P. Aufmuth; C. Aulbert; B. E. Aylott; S. Babak; P. Baker; G. Ballardin; S. Ballmer; D. Barker; S. Barnum; F. Barone; B. Barr; P. Barriga; L. Barsotti; M. Barsuglia; M. A. Barton; I. Bartos; R. Bassiri; M. Bastarrika; A. Basti; J. Bauchrowitz; Th S. Bauer; B. Behnke; M. G. Beker; A. S. Bell; A. Belletoile; I. Belopolski; M. Benacquista; A. Bertolini; J. Betzwieser; N. Beveridge; P. T. Beyersdorf; I. A. Bilenko; G. Billingsley; J. Birch; S. Birindelli; R. Biswas; M. Bitossi; M. A. Bizouard; E. Black; J. K. Blackburn; L. Blackburn; D. Blair; B. Bland; M. Blom; O. Bock; T. P. Bodiya; C. Bogan; R. Bondarescu; F. Bondu; L. Bonelli; R. Bonnand; R. Bork; M. Born; V. Boschi; S. Bose; L. Bosi; B. Bouhou; M. Boyle; S. Braccini; C. Bradaschia; P. R. Brady; V. B. Braginsky; J. E. Brau; J. Breyer; D. O. Bridges; A. Brillet; M. Brinkmann; V. Brisson; M. Britzger; A. F. Brooks; D. A. Brown; A. Brummit; R. Budzyński; T. Bulik; H. J. Bulten; A. Buonanno; J. Burguet-Castell; O. Burmeister; D. Buskulic; C. Buy; R. L. Byer; L. Cadonati; G. Cagnoli; J. Cain; E. Calloni; J. B. Camp; E. Campagna; P. Campsie; J. Cannizzo; K. Cannon; B. Canuel; J. Cao; C. Capano; F. Carbognani; S. Caride; S. Caudill; M. Cavaglià; F. Cavalier; R. Cavalieri; G. Cella; C. Cepeda; E. Cesarini; O. Chaibi; T. Chalermsongsak; E. Chalkley; P. Charlton; E. Chassande-Mottin; S. Chelkowski; Y. Chen; A. Chincarini; N. Christensen; S. S.Y. Chua; C. T.Y. Chung; S. Chung; F. Clara; D. Clark; J. Clark; J. H. Clayton; F. Cleva; E. Coccia; C. N. Colacino; J. Colas; A. Colla; M. Colombini; R. Conte; D. Cook; T. R. Corbitt; N. Cornish; A. Corsi; C. A. Costa; M. Coughlin; J. P. Coulon; D. M. Coward; D. C. Coyne; J. D.E. Creighton; T. D. Creighton; A. M. Cruise; R. M. Culter; A. Cumming; L. Cunningham; E. Cuoco; K. Dahl; S. L. Danilishin; R. Dannenberg; S. D'Antonio; K. Danzmann; K. Das; V. Dattilo; B. Daudert; H. Daveloza; M. Davier; G. Davies; E. J. Daw; R. Day; T. Dayanga; R. De Rosa; D. DeBra; G. Debreczeni; J. Degallaix; M. Del Prete; T. Dent; V. Dergachev; R. DeRosa; R. DeSalvo; S. Dhurandhar; L. Di Fiore; A. Di Lieto; I. Di Palma; M. Di Paolo Emilio; A. Di Virgilio; M. Díaz; A. Dietz; F. Donovan; K. L. Dooley; S. Dorsher; E. S.D. Douglas; M. Drago; R. W.P. Drever; J. C. Driggers; J. C. Dumas; S. Dwyer; T. Eberle; M. Edgar; M. Edwards; A. Effler; P. Ehrens; R. Engel; T. Etzel; M. Evans; T. Evans; M. Factourovich; V. Fafone; S. Fairhurst; Y. Fan; B. F. Farr; D. Fazi; H. Fehrmann; D. Feldbaum; I. Ferrante; F. Fidecaro; L. S. Finn; I. Fiori; R. Flaminio; M. Flanigan; S. Foley; E. Forsi; L. A. Forte; N. Fotopoulos; J. D. Fournier; J. Franc; S. Frasca; F. Frasconi; M. Frede; M. Frei; Z. Frei; A. Freise; R. Frey; T. T. Fricke; D. Friedrich; P. Fritschel; V. V. Frolov; P. Fulda; M. Fyffe; M. Galimberti; L. Gammaitoni; J. Garcia; J. A. Garofoli; F. Garufi; M. E. Gáspár; G. Gemme; E. Genin; A. Gennai; S. Ghosh; J. A. Giaime; S. Giampanis; K. D. Giardina; A. Giazotto; C. Gill; E. Goetz; L. M. Goggin; G. González; M. L. Gorodetsky; S. Goßler; R. Gouaty; C. Graef; M. Granata; A. Grant; S. Gras; C. Gray; R. J.S. Greenhalgh; A. M. Gretarsson; C. Greverie; R. Grosso; H. Grote; S. Grunewald; G. M. Guidi; C. Guido; R. Gupta; E. K. Gustafson; R. Gustafson; B. Hage; J. M. Hallam; D. Hammer; G. Hammond; J. Hanks; C. Hanna; J. Hanson; J. Harms; G. M. Harry; I. W. Harry; E. D. Harstad; M. T. Hartman; K. Haughian; K. Hayama; J. F. Hayau; T. Hayler; J. Heefner; H. Heitmann; P. Hello; M. A. Hendry; I. S. Heng; A. W. Heptonstall; V. Herrera; M. Hewitson; S. Hild; D. Hoak; K. A. Hodge; K. Holt; T. Hong; S. Hooper; D. J. Hosken; J. Hough; E. J. Howell; D. Huet; B. Hughey; S. Husa; S. H. Huttner; D. R. Ingram; R. Inta; T. Isogai; A. Ivanov; P. Jaranowski; W. W. Johnson; D. I. Jones; G. Jones; R. Jones; L. Ju; P. Kalmus; V. Kalogera; S. Kandhasamy; J. B. Kanner; E. Katsavounidis; W. Katzman; K. Kawabe; S. Kawamura; F. Kawazoe; W. Kells; M. Kelner; D. G. Keppel; A. Khalaidovski; F. Y. Khalili; E. A. Khazanov; H. Kim; N. Kim; P. J. King; D. L. Kinzel; J. S. Kissel; S. Klimenko; V. Kondrashov; R. Kopparapu; S. Koranda; W. Z. Korth; I. Kowalska; D. Kozak; V. Kringel; S. Krishnamurthy; B. Krishnan; A. Królak; G. Kuehn; R. Kumar; P. Kwee; M. Landry; B. Lantz; N. Lastzka; A. Lazzarini; P. Leaci; J. Leong; I. Leonor; N. Leroy; N. Letendre; J. Li; T. G.F. Li; N. Liguori; P. E. Lindquist; N. A. Lockerbie; D. Lodhia; M. Lorenzini; V. Loriette; M. Lormand; G. Losurdo; P. Lu; J. Luan; M. Lubinski; H. Lück; A. P. Lundgren; E. Macdonald; B. Machenschalk; M. MacInnis; M. Mageswaran; K. Mailand; E. Majorana; I. Maksimovic; N. Man; I. Mandel; V. Mandic; M. Mantovani; A. Marandi; F. Marchesoni; F. Marion; S. Márka; Z. Márka; E. Maros; J. Marque; F. Martelli; I. W. Martin; R. M. Martin; J. N. Marx; K. Mason; A. Masserot; F. Matichard; L. Matone; R. A. Matzner; N. Mavalvala; R. McCarthy; D. E. McClelland; S. C. McGuire; G. McIntyre; D. J.A. McKechan; G. Meadors; M. Mehmet; T. Meier; A. Melatos; A. C. Melissinos; G. Mendell; R. A. Mercer; L. Merill; S. Meshkov; C. Messenger; M. S. Meyer; H. Miao; C. Michel; L. Milano; J. Miller; Y. Minenkov; Y. Mino; V. P. Mitrofanov; G. Mitselmakher; R. Mittleman; O. Miyakawa; B. Moe; P. Moesta; M. Mohan; S. D. Mohanty; S. R.P. Mohapatra; D. Moraru; G. Moreno; N. Morgado; A. Morgia; S. Mosca; V. Moscatelli; K. Mossavi; B. Mours; C. M. Mow-Lowry; G. Mueller; S. Mukherjee; A. Mullavey; H. Müller-Ebhardt; J. Munch; P. G. Murray; T. Nash; R. Nawrodt; J. Nelson; I. Neri; G. Newton; E. Nishida; A. Nishizawa; F. Nocera; D. Nolting; E. Ochsner; J. O'Dell; G. H. Ogin; R. G. Oldenburg; B. O'Reilly; R. O'Shaughnessy; C. Osthelder; C. D. Ott; D. J. Ottaway; R. S. Ottens; H. Overmier; B. J. Owen; A. Page; G. Pagliaroli; L. Palladino; C. Palomba; Y. Pan; C. Pankow; F. Paoletti; M. A. Papa; A. Parameswaran; S. Pardi; M. Parisi; A. Pasqualetti; R. Passaquieti; D. Passuello; P. Patel; D. Pathak; M. Pedraza; L. Pekowsky; S. Penn; C. Peralta; A. Perreca; G. Persichetti; M. Phelps; M. Pichot; M. Pickenpack; F. Piergiovanni; M. Pietka; L. Pinard; I. M. Pinto; M. Pitkin; H. J. Pletsch; M. V. Plissi; J. Podkaminer; R. Poggiani; J. Pöld; F. Postiglione; M. Prato; V. Predoi; L. R. Price; M. Prijatelj; M. Principe; S. Privitera; R. Prix; G. A. Prodi; L. Prokhorov; O. Puncken; M. Punturo; P. Puppo; V. Quetschke; F. J. Raab; D. S. Rabeling; I. Rácz; H. Radkins; P. Raffai; M. Rakhmanov; C. R. Ramet; B. Rankins; P. Rapagnani; V. Raymond; V. Re; K. Redwine; C. M. Reed; T. Reed; T. Regimbau; S. Reid; D. H. Reitze; F. Ricci; R. Riesen; K. Riles; P. Roberts; N. A. Robertson; F. Robinet; C. Robinson; E. L. Robinson; A. Rocchi; S. Roddy; L. Rolland; J. Rollins; J. D. Romano; R. Romano; J. H. Romie; D. Rosińska; C. Röver; S. Rowan; A. Rüdiger; P. Ruggi; K. Ryan; S. Sakata; M. Sakosky; F. Salemi; M. Salit; L. Sammut; L. Sancho de la Jordana; V. Sandberg; V. Sannibale; L. Santamaría; I. Santiago-Prieto; G. Santostasi; S. Saraf; B. Sassolas; B. S. Sathyaprakash; S. Sato; M. Satterthwaite; P. R. Saulson; R. Savage; R. Schilling; S. Schlamminger; R. Schnabel; R. M.S. Schofield; B. Schulz; B. F. Schutz; P. Schwinberg; J. Scott; S. M. Scott; A. C. Searle; F. Seifert; D. Sellers; A. S. Sengupta; D. Sentenac; A. Sergeev; D. A. Shaddock; M. Shaltev; B. Shapiro; P. Shawhan; T. Shihan Weerathunga; D. H. Shoemaker; A. Sibley; X. Siemens; D. Sigg; A. Singer; L. Singer; A. M. Sintes; G. Skelton; B. J.J. Slagmolen; J. Slutsky; J. R. Smith; M. R. Smith; N. D. Smith; R. Smith; K. Somiya; B. Sorazu; J. Soto; F. C. Speirits; L. Sperandio; M. Stefszky; A. J. Stein; J. Steinlechner; S. Steinlechner; S. Steplewski; A. Stochino; R. Stone; K. A. Strain; S. Strigin; A. S. Stroeer; R. Sturani; A. L. Stuver; T. Z. Summerscales; M. Sung; S. Susmithan; P. J. Sutton; B. Swinkels; G. P. Szokoly; M. Tacca; D. Talukder; D. B. Tanner; S. P. Tarabrin; J. R. Taylor; R. Taylor; P. Thomas; K. A. Thorne; K. S. Thorne; E. Thrane; A. Thüring; C. Titsler; K. V. Tokmakov; A. Toncelli; M. Tonelli; O. Torre; C. Torres; C. I. Torrie; E. Tournefier; F. Travasso; G. Traylor; M. Trias; K. Tseng; L. Turner; D. Ugolini; K. Urbanek; H. Vahlbruch; B. Vaishnav; G. Vajente; M. Vallisneri; J. F.J. Van Den Brand; C. Van Den Broeck; S. Van Der Putten; M. V. Van Der Sluys; A. A. Van Veggel; S. Vass; M. Vasuth; R. Vaulin; M. Vavoulidis; A. Vecchio; G. Vedovato; J. Veitch; P. J. Veitch; C. Veltkamp; D. Verkindt; F. Vetrano; A. Vicere; A. E. Villar; J. Y. Vinet; H. Vocca; C. Vorvick; S. P. Vyachanin; S. J. Waldman; L. Wallace; A. Wanner; R. L. Ward; M. Was; P. Wei; M. Weinert; A. J. Weinstein; R. Weiss; L. Wen; S. Wen; P. Wessels; M. West; T. Westphal; K. Wette; J. T. Whelan; S. E. Whitcomb; D. White; B. F. Whiting; C. Wilkinson; P. A. Willems; H. R. Williams; L. Williams; B. Willke; L. Winkelmann; W. Winkler; C. C. Wipf; A. G. Wiseman; G. Woan; R. Wooley; J. Worden; J. Yablon; I. Yakushin; H. Yamamoto; K. Yamamoto; H. Yang; D. Yeaton-Massey; S. Yoshida; P. Yu; M. Yvert; M. Zanolin; L. Zhang; Z. Zhang; C. Zhao; N. Zotov; M. E. Zucker; J. Zweizig; R. L. Aptekar; W. V. Boynton; M. S. Briggs; T. L. Cline; V. Connaughton; D. D. Frederiks; N. Gehrels; J. O. Goldsten; D. Golovin; A. J. Van Der Horst; K. C. Hurley; Y. Kaneko; A. Von Kienlin; C. Kouveliotou; H. A. Krimm; L. Lin; I. Mitrofanov; M. Ohno; V. D. Pal'shin; A. Rau; A. Sanin; M. S. Tashiro; Y. Terada; K. Yamaoka
  Astrophysical Journal Letters, Volume：734, Number：2, Jun. 2011, [Reviewed]
  Soft gamma repeaters (SGRs) and anomalous X-ray pulsars (AXPs) are thought to be magnetars: neutron stars powered by extreme magnetic fields. These rare objects are characterized by repeated and sometimes spectacular gamma-ray bursts. The burst mechanism might involve crustal fractures and excitation of non-radial modes which would emit gravitational waves (GWs). We present the results of a search for GW bursts from six galactic magnetars that is sensitive to neutron star f-modes, thought to be the most efficient GW emitting oscillatory modes in compact stars. One of them, SGR 0501+4516, is likely 1kpc from Earth, an order of magnitude closer than magnetars targeted in previous GW searches. A second, AXP 1E 1547.0-5408, gave a burst with an estimated isotropic energy >
  1044erg which is comparable to the giant flares. We find no evidence of GWs associated with a sample of 1279 electromagnetic triggers from six magnetars occurring between 2006 November and 2009 June, in GW data from the LIGO, Virgo, and GEO600 detectors. Our lowest model-dependent GW emission energy upper limits for band- and time-limited white noise bursts in the detector sensitive band, and for f-mode ringdowns (at 1090Hz), are 3.0 × 1044 d 2 1erg and 1.4 × 10 47 d 2 1erg, respectively, where and d 0501 is the distance to SGR 0501+4516. These limits on GW emission from f-modes are an order of magnitude lower than any previous, and approach the range of electromagnetic energies seen in SGR giant flares for the first time. © 2011. The American Astronomical Society. All rights reserved.
  English, Scientific journal
  DOI：https://doi.org/10.1088/2041-8205/734/2/L35
  DOI ID：10.1088/2041-8205/734/2/L35, ISSN：2041-8205, ORCID：78692603, SCOPUS ID：79959405183
• Spectral Cross-Calibration of the Konus-Wind, the Suzaku/WAM, and the Swift/BAT Data Using Gamma-Ray Bursts　　　　　　　　　　　　　　　
  Takanori Sakamoto; Valentin Pal'Shin; Kazutaka Yamaoka; Masarlori Ohno; Goro Sato; Rafail Aptekar; Scott D. Barthelmy; Wayne H. Baumgartner; Jay R. Cummings; Edward E. Fenimore; Dmitry Frederiks; Neil Gehrels; Sergey Golenetskii; Hans A. Krimm; Craig B. Markwardt; Kaori Onda; David M. Palmer; Ann M. Parsons; Michael Stamatikos; Satoshi Sugita; Makoto Tashiro; Jack Tueller; Tilan N. Ukwatta
  PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN, Volume：63, Number：1, First page：215, Last page：277, Feb. 2011, [Reviewed]
  We report on the spectral cross-calibration results of the Konus-Wind, the Suzaku/WAM, and the Swift/BAT instruments using simultaneously observed gamma-ray bursts (GRBs). This is the first attempt to use simultaneously observed GRBs as a spectral calibration source to understand systematic problems among the instruments. Based on these joint spectral fits, we find that (1) although a constant factor (a normalization factor) agrees within 20% among the instruments, the BAT constant factor shows a systematically smaller value by 10%-20% compared to that of Konus-Wind, (2) there is a systematic trend that the low-energy photon index becomes steeper by 0.1-0.2 and E-peak becomes systematically higher by 10%-20% when including the BAT data in the joint fits, and (3) the high-energy photon index agrees within 0.2 among the instruments. Our results show that cross-calibration based on joint spectral analysis is an important step to understanding the instrumental effects that could be affecting the scientific results from the GRB prompt emission data.
  OXFORD UNIV PRESS, English, Scientific journal
  DOI：https://doi.org/10.1093/pasj/63.1.215
  DOI ID：10.1093/pasj/63.1.215, ISSN：0004-6264, eISSN：2053-051X, Web of Science ID：WOS:000288283700023
• SUZAKU DIAGNOSTICS OF THE ENERGETICS IN THE LOBES OF THE GIANT RADIO GALAXY 3C 35　　　　　　　　　　　　　　　
  Naoki Isobe; Hiromi Seta; Poshak Gandhi; Makoto S. Tashiro
  ASTROPHYSICAL JOURNAL, Volume：727, Number：2, Feb. 2011, [Reviewed]
  The Suzaku observation of a giant radio galaxy 3C 35 revealed faint extended X-ray emission, associated with its radio lobes and/or host galaxy. After careful subtraction of the X-ray and non-X-ray background and contaminating X-ray sources, the X-ray spectrum of the faint emission was reproduced by a sum of the power-law (PL) and soft thermal components. The soft component was attributed to the thermal plasma emission from the host galaxy. The photon index of the PL component, Gamma = 1.35(-0.86-0.10)(+0.56+0.11),where the first and second errors represent the statistical and systematic ones, was found to agree with the synchrotron radio index from the lobes, Gamma(R) = 1.7. Thus, the PL component was attributed to the inverse Compton (IC) X-rays from the synchrotron electrons in the lobes. The X-ray flux density at 1 keV was derived as 13.6 +/- 5.4(-3.6)(+4.0) nJy with the photon index fixed at the radio value. The X-ray surface brightness from these lobes (similar to 0.2 nJy arcmin(-2)) is lowest among the lobes studied through the IC X-ray emission. In combination with the synchrotron radio flux density, 7.5 +/- 0.2 Jy at 327.4 MHz, the electron energy density spatially averaged over the lobes was evaluated to be the lowest among those radio galaxies, as u(e) = (5.8 +/- 2.3(-1.7)(+1.9)) x 10(-14) erg cm(-3) over the electron Lorentz factor of 10(3) - 10(5). The magnetic energy density was calculated as u(m) = (3.1(-1.0-0.9)(+2.5+1.4)) x 10(-14) erg cm(-3), corresponding to the magnetic field strength of 0.88(-0.16-0.14)(+0.31+0.19) mu G. These results suggest that the energetics in the 3C 35 lobes are nearly consistent with equipartition between the electrons and magnetic fields.
  IOP PUBLISHING LTD, English, Scientific journal
  DOI：https://doi.org/10.1088/0004-637X/727/2/82
  DOI ID：10.1088/0004-637X/727/2/82, ISSN：0004-637X, eISSN：1538-4357, Web of Science ID：WOS:000286662000021
• WIDGET: System Performance and GRB Prompt Optical Observations　　　　　　　　　　　　　　　
  Yuji Urata; Makoto S. Tashiro; Toru Tamagawa; Fumihiko Usui; Makoto Kuwahara; Hungmiao Lin; Shoichi Kageyama; Wataru Iwakiri; Takako Sugasahara; Kazuki Takahara; Natsuki Kodaka; Keiichi Abe; Keisuke Masuno; Kaori Onda
  PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN, Volume：63, Number：1, First page：137, Last page：146, Feb. 2011, [Reviewed]
  The WIDeField telescope for Gamma-ray burst Early Timing (WIDGET) is used for a fully automated, ultrawide-field survey aimed at detecting the prompt optical emission associated with Gamma-ray Bursts (GRBs). WIDGET surveys the HETE-2 and Swift/BAT pointing directions, covering a total field of view of 62 x 62 every 10 secounds using a unfiltered system. This monitoring survey allows the exploration of optical emission before the gamma-ray trigger. The unfiltered magnitude is well converted to the SDSS r' system at a 0.1 mag level. Since 2004, WIDGET has made a total of ten simultaneous and one pre-trigger GRB observations. The efficiency of synchronized observations with HETE-2 is four-times better than that of Swift. There has been no bright optical emission similar to that from GRB 080319B. A statistical analysis implies that GRB 080319B is a rare event. This paper summarizes the design and operation of the WIDGET system and the simultaneous GRB observations obtained with this instrument.
  OXFORD UNIV PRESS, English, Scientific journal
  DOI：https://doi.org/10.1093/pasj/63.1.137
  DOI ID：10.1093/pasj/63.1.137, ISSN：0004-6264, eISSN：2053-051X, Web of Science ID：WOS:000288283700017
• The third interplanetary network　　　　　　　　　　　　　　　
  K. Hurley; S. Golenetskii; R. Aptekar; E. Mazets; V. Pal'shin; D. Frederiks; I. G. Mitrofanov; D. Golovin; A. Kozyrev; M. Litvak; A. B. Sanin; W. Boynton; C. Fellows; K. Harshman; R. Starr; A. Von Kienlin; A. Rau; K. Yamaoka; M. Ohno; Y. Fukazawa; T. Takahashi; M. Tashiro; Y. Terada; T. Murakami; K. Makishima; S. Barthelmy; J. Cummings; N. Gehrels; H. Krimm; T. Cline; J. Goldsten; E. Del Monte; M. Feroci; M. Marisaldi; M. Briggs; V. Connaughton; C. Meegan; D. M. Smith; C. Wigger; W. Hajdas
  AIP Conference Proceedings, Volume：1358, First page：385, Last page：388, 2011, [Reviewed]
  The 3rd interplanetary network (IPN), which has been in operation since 1990, presently consists of 9 spacecraft: AGILE, Fermi, RHESSI, Suzaku, and Swift, in low Earth orbit
  INTEGRAL, in eccentric Earth orbit with apogee 0.5 light-seconds
  Wind, up to ∼7 light-seconds from Earth
  MESSENGER, en route to Mercury
  and Mars Odyssey, in orbit around Mars. The IPN operates as a full-time, all-sky monitor for transients down to a threshold of about 6×10-7 erg cm-2 or 1 photon cm-2 s-1. It detects ∼335 cosmic gamma-ray bursts per year. These events are generally not the same ones detected by narrower field of view instruments such as Swift, INTEGRAL IBIS, SuperAGILE, and MAXI
  the localization accuracy is in the several arcminute and above range. The data are publicly available and can be utilized for a wide variety of studies. © 2011 American Institute of Physics.
  English, International conference proceedings
  DOI：https://doi.org/10.1063/1.3621810
  DOI ID：10.1063/1.3621810, ISSN：0094-243X, SCOPUS ID：80052483845
• Suzaku observations of the radio galaxy Fornax A west lobe　　　　　　　　　　　　　　　
  Hiromi Seta; Makoto S. Tashiro; Naoki Isobe
  JETS AT ALL SCALES, Number：275, First page：184, Last page：185, 2011, [Reviewed]
  We performed mapping observations of the Fornax A west lobe with Suzaku in order to measure X-ray brightness distribution. Thanks to the low and stable background of Suzaku, we succeeded in detecting the faint diffuse X-ray emission from the west lobe. Performing careful corrections to the obtained images, we finally measured the X-ray brightness profile extending over the lobe. By comparing the X-ray and radio profiles, the magnetic field found to be fairly constant at similar to 1 mu G over the lobe, while the electron energy distribution is suggested to concentrate on the lobe center.
  CAMBRIDGE UNIV PRESS, English, International conference proceedings
  DOI：https://doi.org/10.1017/S1743921310015966
  DOI ID：10.1017/S1743921310015966, ISSN：1743-9213, Web of Science ID：WOS:000304974800039
• The Time Assignment System of ASTRO-H　　　　　　　　　　　　　　　
  Tomomi Kouzu; Kaori Iwase; Yuki Mishima; Yukikatsu Terada; Takayuki Yuasa; Yoshitaka Ishisaki; Makoto S. Tashiro; Motohide Kokubun; Masanobu Ozaki; Masaharu Nomachi; Tadayuki Takahashi
  2011 IEEE NUCLEAR SCIENCE SYMPOSIUM AND MEDICAL IMAGING CONFERENCE (NSS/MIC), First page：163, Last page：166, 2011, [Reviewed]
  ASTRO-H is an X-ray astronomy satellite to be launched in 2014. The data acquisition system of this mission is realized with a standard network protocol, SpaceWire. Although the protocol itself is well designed, a new concept to grantee the quality of service will be installed to the ASTRO-H data acquisition system. Therefore, the verification of the design of the concept is essential in the initial phase of the development. The time assignment function is one of the important issues for the SpaceWire development. The accuracy of the absolute time of about 30 mu s is required from science goals. The key point of the time assignment with SpaceWire network in the ASTRO-H system is how accurately sharing the time information. In this paper, our design of the time distribution and assignment system for ASTRO-H is shown. The results of our measurements of timing accuracy are also presented to show that the design will fulfill the goal of absolute timing accuracy.
  IEEE, English, International conference proceedings
  DOI：https://doi.org/10.1109/NSSMIC.2011.6154471
  DOI ID：10.1109/NSSMIC.2011.6154471, ISSN：1082-3654, ORCID：34407208, SCOPUS ID：84863348846, Web of Science ID：WOS:000304755600030
• Abundance Patterns in the Interstellar Medium of the S0 Galaxy NGC 1316 (Fornax A) Revealed with Suzaku　　　　　　　　　　　　　　　
  Saori Konami; Kyoko Matsushita; Ryo Nagino; Makoto S. Tashiro; Toru Tamagawa; Kazuo Makishima
  PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN, Volume：62, Number：6, First page：1435, Last page：1443, Dec. 2010, [Reviewed]
  The Suzaku X-ray satellite observed the nearby S0 galaxy NGC 1316, a merger remnant aged 3 Gyr. The total good exposure time was 48.7 ks. The spectra were well represented by a two-temperature thermal model for the interstellar medium (ISM) plus a power-law model. The cool and hot temperatures of the thermal model were 0.48 +/- 0.03 and 0.92 +/- 0.04 keV, respectively. The excellent spectral sensitivity of Suzaku enables us for the first time to measure the metal abundances of O, Ne, Mg, Si, and Fe in the ISM. The resultant abundance pattern of O, Ne, Mg, Si, and Fe is close to that of the new solar abundance determined by Lodders (2003, ApJ, 591, 1220). The measured abundance pattern is compared with those of elliptical galaxies and an S0 galaxy, observed with Suzaku. Considering metal-enrichment from present Type la supernovae, the near-solar abundance pattern of the ISM in NGC 1316 indicates an enhanced alpha/Fe ratio of stellar materials in the entire galaxy, like in giant elliptical galaxies.
  OXFORD UNIV PRESS, English, Scientific journal
  DOI：https://doi.org/10.1093/pasj/62.6.1435
  DOI ID：10.1093/pasj/62.6.1435, ISSN：0004-6264, eISSN：2053-051X, Web of Science ID：WOS:000286360100011
• The high-resolution X-ray microcalorimeter Spectrometer system for the SXS on ASTRO-H
  Kazuhisa Mitsuda, Richard; L. Kelley; Kevin R. Boyce; Gregory V. Brown; Elisa Costantini; Michael J. DiPirro; Yuichiro Ezoe; Ryuichi Fujimoto; Keith C. Gendreau; Jan Willem Den Herder; Akio Hoshino; Yoshitaka Ishisaki; Caroline A. Kilbourne; Shunji Kitamoto; Dan McCammon; Masahide Murakami; Hiroshi Murakami; Mina Ogawa; Takaya Ohashi; Atsushi Okamoto; Stéphane Paltani; Martin Pohl; F. Scott Porter; Yoichi Sato; Keisuke Shinozaki; Peter J. Shirron; Gary A. Sneiderman; Hiroyuki Sugita; Andrew Szymkowiak; Yoh Takei; Toru Tamagawa; Makoto Tashiro; Yukikatsu Terada; Masahiro Tsujimoto; Cor De Vries; Hiroya Yamaguchi; Noriko Y. Yamasaki
  Proceedings of SPIE - The International Society for Optical Engineering, Volume：7732, Oct. 2010
  We present the science and an overview of the Soft X-ray Spectrometer onboard the ASTRO-H mission with emphasis on the detector system. The SXS consists of X-ray focusing mirrors and a microcalorimeter array and is developed by international collaboration lead by JAXA and NASA with European participation. The detector is a 6×6 format microcalorimeter array operated at a cryogenic temperature of 50 mK and covers a 3′ ×3′ filed of view of the X-ray telescope of 5.6 m focal length. We expect an energy resolution better than 7 eV (FWHM, requirement) with a goal of 4 eV. The effective area of the instrument will be 225 cm2 at 7 keV; by a factor of about two larger than that of the X-ray microcalorimeter on board Suzaku. One of the main scientific objectives of the SXS is to investigate turbulent and/or macroscopic motions of hot gas in clusters of galaxies. © 2010 SPIE.
  DOI：https://doi.org/10.1117/12.856778
  DOI ID：10.1117/12.856778, ISSN：0277-786X, SCOPUS ID：77957866598
• A Catalog of Suzaku/WAM Hard X-Ray Solar Flares　　　　　　　　　　　　　　　
  Akira Endo; Takashi Minoshima; Kouichi Morigami; Masanobu Suzuki; Atsushi Shimamori; Yumi Sato; Yukikatsu Terada; Makoto S. Tashiro; Yuji Urata; Eri Sonoda; Kazutaka Yamaoka; Satoshi Sugita; Kyoko Watanabe
  PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN, Volume：62, Number：5, First page：1341, Last page：1349, Oct. 2010, [Reviewed]
  We developed a catalog of solar flares in the hard X-ray band observed with the Wide-band All-sky Monitor (WAM) onboard the Suzaku satellite between 2005 July and 2009 November. During this period, 105 solar flares (GOES class X: 13, M: 29, C: 47, B: 16) were detected with WAM, including 10% of GOES-class C events reported during the same period. The observed photon flux ranged between 9 x 10(-5) and 9 x 10(-1) photons s(-1) cm(-2) keV(-1) at 100 keV. The averaged hard X-ray spectrum for each solar flare was evaluated for 70 of the 105 events, and 43 of them were well fitted with a single power-law model with a photon index ranging between -7 and -3. We observed a weak trend where events with longer durations exhibited harder spectral slopes.
  OXFORD UNIV PRESS, English, Scientific journal
  DOI：https://doi.org/10.1093/pasj/62.5.1341
  DOI ID：10.1093/pasj/62.5.1341, ISSN：0004-6264, eISSN：2053-051X, Web of Science ID：WOS:000283885700024
• EVIDENCE OF NON-THERMAL X-RAY EMISSION FROM RADIO LOBES OF CYGNUS A
  Y. Yaji; M. S. Tashiro; N. Isobe; M. Kino; K. Asada; H. Nagai; S. Koyama; M. Kusunose
  The Astrophysical Journal, Volume：714, Number：1, First page：37, Last page：44, May 2010, [Reviewed]
  Using deep Chandra Advanced CCD Imaging Spectrometer (ACIS) observation data for Cygnus A, we report evidence of non-thermal X-ray emission from radio lobes surrounded by a rich intracluster medium (ICM). The diffuse X-ray emission, which is associated with the eastern and western radio lobes, was observed in a 0.7-7 keV Chandra ACIS image. The lobe spectra are reproduced with not only a single-temperature Mekal model, such as that of the surrounding ICM component, but also an additional power-law (PL) model. The X-ray flux densities of PL components for the eastern and western lobes at 1 keV are derived as 77.7+28.9 -31.9 nJy and 52.4+42.9 -42.4 nJy, respectively, and the photon indices are 1.69 +0.07 -0.13 and 1.84+2.90 -0.12, respectively. The non-thermal component is considered to be produced via the inverse Compton (IC) process, as is often seen in the X-ray emission from radio lobes. From a re-analysis of radio observation data, the multiwavelength spectra strongly suggest that the seed photon source of the IC X-rays includes both cosmic microwave background radiation and synchrotron radiation from the lobes. The derived parameters indicate significant dominance of the electron energy density over the magnetic field energy density in the Cygnus A lobes under the rich ICM environment. © 2010. The American Astronomical Society. All rights reserved..
  IOP Publishing, English, Scientific journal
  DOI：https://doi.org/10.1088/0004-637x/714/1/37
  DOI ID：10.1088/0004-637x/714/1/37, ISSN：0004-637X, eISSN：1538-4357, SCOPUS ID：77951142237
• Timing analysis of unusual GRB 090709A observed by Suzaku Wide-band All sky Monitor　　　　　　　　　　　　　　　
  W. Iwakiri; M. Ohno; T. Kamae; Y. E. Nakagawa; Y. Terada; M. S. Tashiro; A. Yoshida; K. Yamaoka; K. Makishima
  AIP Conference Proceedings, Volume：1279, First page：89, Last page：92, 2010, [Reviewed]
  A result of a joint timing analysis is presented for prompt emission of long-duration (T90 = 81 s) GRB 090709A with Swift Burst Alert Telescope (Swift/BAT), Suzaku Wide-band All-sky Monitor (Suzaku/WAM) and Konus-Wind over an energy range from 15 keV to 5 MeV. It was reported that multi-peaked GRB 090709A exhibited a possible periodic behavior with a period of about 8 s which is comparable to typical time scale of soft gamma-ray repeaters. However, the periodicity is still marginal in detailed analysis with Swift/BAT and GRB090709A exhibited a typical afterglow [1] [2]. To investigate significance of the periodicity more quantitatively, we performed a detailed timing analysis on all the lightcurves obtained with Suzaku/WAM, Swift/BAT, and Konus-Wind evaluating their underlying trend, red noise and white noise. © 2010 American Institute of Physics.
  English, International conference proceedings
  DOI：https://doi.org/10.1063/1.3509358
  DOI ID：10.1063/1.3509358, ISSN：0094-243X, SCOPUS ID：78649876025
• Soft Gamma-ray Detector for the ASTRO-H Mission　　　　　　　　　　　　　　　
  Hiroyasu Tajima; Roger Blandford; Teruaki Enoto; Yasushi Fukazawa; Kirk Gilmore; Tuneyoshi Kamae; Jun Kataoka; Madoka Kawaharada; Motohide Kokubun; Philippe Laurent; Francois Lebrun; Olivier Limousin; Greg Madejski; Kazuo Makishima; Tsunefumi Mizuno; Kazuhiro Nakazawa; Masanori Ohno; Masayuki Ohta; Goro Sato; Rie Sato; Hiromitsu Takahashi; Tadayuki Takahashi; Takaaki Tanaka; Makoto Tashiro; Yukikatsu Terada; Yasunobu Uchiyama; Shin Watanabe; Kazutaka Yamaoka; Daisuke Yonetoku
  SPACE TELESCOPES AND INSTRUMENTATION 2010: ULTRAVIOLET TO GAMMA RAY, Volume：7732, 2010, [Reviewed]
  ASTRO-H is the next generation JAXA X-ray satellite, intended to carry instruments with broad energy coverage and exquisite energy resolution. The Soft Gamma-ray Detector (SGD) is one of ASTRO-H instruments and will feature wide energy band (40-600 keV) at a background level 10 times better than the current instruments on orbit. SGD is complimentary to ASTRO-H's Hard X-ray Imager covering the energy range of 5-80 keV. The SGD achieves low background by combining a Compton camera scheme with a narrow field-of-view active shield where Compton kinematics is utilized to reject backgrounds. The Compton camera in the SGD is realized as a hybrid semiconductor detector system which consists of silicon and CdTe (cadmium telluride) sensors. Good energy resolution is afforded by semiconductor sensors, and it results in good background rejection capability due to better constraints on Compton kinematics. Utilization of Compton kinematics also makes the SGD sensitive to the gamma-ray polarization, opening up a new window to study properties of gamma-ray emission processes. The ASTRO-H mission is approved by ISAS/JAXA to proceed to a detailed design phase with an expected launch in 2014. In this paper, we present science drivers and concept of the SGD instrument followed by detailed description of the instrument and expected performance.
  SPIE-INT SOC OPTICAL ENGINEERING, English, International conference proceedings
  DOI：https://doi.org/10.1117/12.857531
  DOI ID：10.1117/12.857531, ISSN：0277-786X, Web of Science ID：WOS:000285506200034
• The third interplanetary network　　　　　　　　　　　　　　　
  K. Hurley; S. Golenetskii; R. Aptekar; E. Mazets; V. Pal'shin; D. Frederiks; I. G. Mitrofanov; D. Golovin; M. L. Litvak; A. B. Sanin; W. Boynton; C. Fellows; K. Harshman; R. Starr; D. M. Smith; C. Wigger; W. Hajdas; A. Von Kienlin; A. Rau; K. Yamaoka; M. Ohno; T. Takahashi; Y. Fukazawa; M. Tashiro; Y. Terada; T. Murakami; K. Makishima; S. Barthelmy; T. Cline; J. Cummings; N. Gehrels; H. Krimm; J. Goldsten; E. Del Monte; M. Feroci; M. Marisaldi; M. Briggs; V. Connaughton; C. Meegan
  AIP Conference Proceedings, Volume：1279, First page：330, Last page：333, 2010, [Reviewed]
  The 3rd interplanetary network (IPN), which has been in operation since 1990, presently consists of 9 spacecraft: AGILE, Fermi, RHESSI, Suzaku, and Swift, in low Earth orbit
  INTEGRAL, in eccentric Earth orbit with apogee 0.5 light-seconds
  Wind, up to ∼7 light-seconds from Earth
  MESSENGER, en route to Mercury
  and Mars Odyssey, in orbit around Mars. The IPN operates as a full-time, all-sky monitor for transients down to a threshold of about 6 × 10-7 erg cm-2 or 1 photoncm-2 s-1. It detects ∼346 cosmic gamma-ray bursts per year. These events are generally not the same ones detected by narrower field of view instruments such as Swift, INTEGRAL IBIS, and SuperAGILE
  the localization accuracy is in the several arcminute and above range. The uses of the IPN data are described. © 2010 American Institute of Physics.
  English, International conference proceedings
  DOI：https://doi.org/10.1063/1.3509301
  DOI ID：10.1063/1.3509301, ISSN：0094-243X, SCOPUS ID：78649890599
• The detector subsystem for the SXS instrument on the Astro-H observatory　　　　　　　　　　　　　　　
  F. S. Porter; J. S. Adams; G. V. Brown; J. A. Chervenak; M. P. Chiao; R. Fujimoto; Y. Ishisaki; R. L. Kelley; C. A. Kilbourne; D. McCammon; K. Mitsuda; T. Ohashi; A. E. Szymkowiak; Y. Takei; M. Tashiro; N. Yamasaki
  Proceedings of SPIE - The International Society for Optical Engineering, Volume：7732, 2010, [Reviewed]
  The Soft X-ray Spectrometer (SXS) instrument on the Astro-H observatory is based on a 36 pixel x-ray calorimeter array cooled to 50 mK in a sophisticated spaceflight cryostat. The SXS is a true spatial-spectral instrument, where each spatially discrete pixel functions as a high-resolution spectrometer. Here we discuss the SXS detector subsystem that includes the detector array, the anticoincidence detector, the first stage amplifiers, the thermal and mechanical staging of the detector, and the cryogenic bias electronics. The design of the SXS detector subsystem has significant heritage from the Suzaku/XRS instrument but has some important modifications that increase performance margins and simplify the focal plane assembly. Notable improvements include x-ray absorbers with significantly lower heat capacity, improved load resistors, improved thermometry, and a decreased sensitivity to thermal radiation. These modifications have yielded an energy resolution of 3.5-4.0 eV FWHM at 6 keV for representative devices in the laboratory, giving considerable margin against the 7 eV instrument requirement. We expect similar performance in flight. © 2010 SPIE.
  English, International conference proceedings
  DOI：https://doi.org/10.1117/12.857888
  DOI ID：10.1117/12.857888, ISSN：0277-786X, SCOPUS ID：77957875609
• Spectral Evolutions in FRED-type Light curves Observed with Suzaku Wideband All-sky Monitor　　　　　　　　　　　　　　　
  Makoto S. Tashiro; Kaori Onda
  DECIPHERING THE ANCIENT UNIVERSE WITH GAMMA-RAY BURSTS, Volume：1279, First page：436, Last page：438, 2010, [Reviewed]
  A study of spectral evolutions of gamma-ray burst (GRB) prompt emissions observed with Suzaku Wide-band All-sky Monitor (WAM) is presented. Thank to the large effective areas, Suzaku-WAM is one of the best instruments to investigate spectral evolutions of the ORB prompt emissions. In general the rise and decay time scales in the light curves are determined by the heating and cooling time scale and geometrical effect of the emission regions. It has been argued that the expected highly relativistic emission regions and its deceleration would produce spectral evolution could cause apparent spectral evolution in the observer frame. However, it is not easy to attribute exponential decays with spectral evolutions to the relativistic effect of the GRB jet. In other words, electron cooling is the key to solve the spectral variations in the exponential decays. This paper focuses the isolated fast-rise-exponential-decay (FRED) type light curve observed with WAM and their spectral evolutions, and revealed an energy dependence of the time constant of the observed exponential decay. The "energy indices" observed from some of the GRBs are consistent with those expected in synchrotron or inverse Compton cooling.
  AMER INST PHYSICS, English, International conference proceedings
  ISSN：0094-243X, Web of Science ID：WOS:000287125000103
• The X-ray Microcalorimeter Spectrometer onboard of IXO　　　　　　　　　　　　　　　
  J. W. den Herder; L. Kelley; K. Mitsuda; L. Piro; S. R. Bandler; P. Bastia; K. R. Boyce; M. Bruin; J. A. Chervenak; L. Colasanti; W. B. Doriese; M. DiPirro; M. E. Eckart; Y. Ezoe; E. Figueroa-Feliciano; L. Ferrari; R. Fujimoto; F. Gatti; K. C. Gendreau; L. Gottardi; R. den Hartog; G. C. Hilton; H. Hoevers; K. D. Irwin; Y. Ishisaki; A. Kashani; C. A. Kilbourne; P. de Korte; J. van der Kuur; C. Macculi; T. Mineo; J. H. Nieland; T. Ohashi; S. Paltani; E. Perinati; F. S. Porter; P. J. Shirron; S. J. Smith; Y. Takei; M. Tashiro; G. Torrioli; M. Tsujimoto; H. van Weers; N. Y. Yamasaki
  SPACE TELESCOPES AND INSTRUMENTATION 2010: ULTRAVIOLET TO GAMMA RAY, Volume：7732, 2010, [Reviewed]
  One of the instruments on the International X-ray Observatory (IXO), under study with NASA, ESA and JAXA, is the X-ray Microcalorimeter Spectrometer (XMS). This instrument, which will provide high spectral resolution images, is based on X-ray micro-calorimeters with Transition Edge Sensor (TES) with absorbers that consist of metal and semi-metal layers and a multiplexed SQUID readout. The requirements for this instrument are demanding. In the central array (40 x 40 pixels) an energy resolution of <2.5 eV is required, whereas the energy resolution of the outer array is more relaxed (approximate to 10 eV) but the detection elements have to be a factor 16 larger in order to keep the number of read-out channels acceptable for a cryogenic instrument. Due to the large collection area of the IXO optics, the XMS instrument must be capable of processing high counting rates, while maintaining the spectral resolution and a low deadtime. In addition, an anti-coincidence detector is required to suppress the particle-induced background. In this paper we will summarize the instrument status and performance. We will describe the results of design studies for the focal plane assembly and the cooling systems. Also the system and its required spacecraft resources will be given.
  SPIE-INT SOC OPTICAL ENGINEERING, English, International conference proceedings
  DOI：https://doi.org/10.1117/12.856018
  DOI ID：10.1117/12.856018, ISSN：0277-786X, eISSN：1996-756X, Web of Science ID：WOS:000285506200045
• Development of BGO active shield for the ASTRO-H soft Gamma-ray Detector
  Hanabata Y; Fukazawa Y; Yamaoka K; Tajima H; Kataoka J; Nakazawa K; Takahashi H; Mizuno T; Ohno M; Kokubun M; Takahashi T; Watanabe S; Tashiro M; Terada Y; Sasaki C; Nakajima K; Mizushima T
  Proceedings of SPIE - The International Society for Optical Engineering, Volume：7732, 2010, [Reviewed]
  Soft Gamma-ray Detector (SGD:40-600 keV) will be mounted on the 6th Japanese X-ray observatory ASTRO-H to be launched in 2014. The main part of the SGD is a Compton camera with a narrow field of view and surrounded by BGO active shields (SGD-BGO). Via this combination, the SGD can achieve sensitivity more than ten times superior to the Suzaku/HXD. The BGO active shield will also function as a gamma-ray burst monitor as proven by the wide-band all-sky monitor (WAM) of the Suzaku/HXD. Avalanche Photodiodes (APDs) are used to read out scintillation lights from the BGO. The size of the former also means we need to focus on collecting light from large, complex-shaped BGO blocks. The significant leakage current of the APD means a lower temperature is preferred to minimize the noise while a higher temperature is preferred to simplify the cooling system. To optimize the BGO shape and the operating temperature, we tested the performance of the BGO readout system with various BGO shapes under different operating temperatures. We also apply waveform sampling by flash-ADC and digital filter instead of a conventional analog filter and ADC scheme to reduce the space and power of the circuit with increased flexibilities. As an active shield, we need to achieve a threshold level of 50-100 keV. Here, we report on the studies of threshold energy of active shield under various conditions and signal processings. © 2010 SPIE.
  International conference proceedings
  DOI：https://doi.org/10.1117/12.856745
  Scopus Citedby：https://www.scopus.com/inward/citedby.uri?partnerID=HzOxMe3b&scp=77957916088&origin=inward
  DOI ID：10.1117/12.856745, ISSN：0277-786X, ORCID：34407187, SCOPUS ID：77957916088
• Time-Resolved Spectral Variability of the Prompt Emission from GRB 070125 Observed with Suzaku/WAM
  Onda, Kaori; Tashiro; Makoto S; Nakagawa; Yujin E; Yamaoka, Kazutaka; Terada, Yukikatsu; Ohno, Masanori; Sugita, Satoshi; Sakamoto, Takanori; Toma, Kenji; Gandhi; Poshak e
  PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN, Volume：62, Number：3, First page：547, Last page：556, 2010, [Reviewed]
  Time-resolved spectral analyses of GRB 070125 with significant photon detections over the MeV regime using Suzaku/WAM data are reported. The prompt emission interval was divided into 10 time regions, and their spectra were reproduced by a Band function or a cutoff power-law model. The spectra show a complex evolution; a soft-hard-soft trend is seen, rather than a typical hard-to-soft monotonic variation. In addition, a flat spectral slope in the low-energy band exceeding the slope expected from a simple synchrotron emission model is suggested in one of the time regions. These results imply that the internal shocks in the relativistic jet of GRB 070125 have different physical conditions. There is a possible excess at similar to 2.2 MeV in the spectrum of 33 seconds after the trigger at a significant level of approximate to 98.5%, where the continuum spectrum is not reproduced by the Band function. These properties are only shown during the short prompt time interval of the prompt emission, and emphasize the utility of the Suzaku/WAM for the study of gamma-ray bursts.
  ASTRONOMICAL SOC JAPAN, Scientific journal
  DOI：https://doi.org/10.1093/pasj/62.3.547
  DOI ID：10.1093/pasj/62.3.547, ISSN：0004-6264, eISSN：2053-051X
• Hard X-ray and gamma-ray detector for ASTRO-H based on Si and CdTe imaging sensors
  Kokubun M; Watanabe S; Nakazawa K; Tajima H; Fukazawa Y; Takahashi T; Kataoka J; Kamae T; Katagiri H; Madejski G.M; Makishima K; Mizuno T; Ohno M; Sato R; Takahashi H; Tanaka T; Tashiro M; Terada Y; Yamaoka K
  Nuclear Instruments and Methods in Physics Research, Section A: Accelerators, Spectrometers, Detectors and Associated Equipment, Volume：623, Number：1, First page：425, Last page：427, 2010, [Reviewed]
  We have been developing a hard X-ray imager and soft gamma-ray detector as on board instruments of the ASTRO-H mission. The Hard X-ray Imager (HXI) is one of the three focal plane detectors of ASTRO-H, which is aimed to realize the focusing imaging of hard X-ray photons in combination with hard X-ray telescopes. By use of the hybrid structure composed of double-sided silicon strip detectors and a cadmium telluride strip detector, it fully covers the energy range up to 80 keV with a high quantum efficiency. High spatial resolutions of 250μm pitch and energy resolutions of 12 keV (FWMH) are at the same time achieved with low noise front-end ASICs. The Soft Gamma-ray Detector (SGD) is a novel and unique detector which is characterized by semiconductor Compton cameras surrounded by narrow field-of-view active shields, and covers a higher energy range (30600 keV) than that of HXI. It consists of four Compton Cameras constructed with many layers of Silicon and CdTe pad detectors. With its multi-layer structure and Compton reconstruction capability, in addition to the BGO active shields read by Avalanche photo-diodes, this detector will achieve an extremely high background rejection efficiency in the orbit. We report the current status of hardware development including the design requirement, expected performance, and technical readinesses of key technologies. © 2010 Elsevier B.V. All rights reserved.
  International conference proceedings
  DOI：https://doi.org/10.1016/j.nima.2010.03.024
  Scopus Citedby：https://www.scopus.com/inward/citedby.uri?partnerID=HzOxMe3b&scp=77957846499&origin=inward
  DOI ID：10.1016/j.nima.2010.03.024, ISSN：0168-9002, ORCID：34407173, SCOPUS ID：77957846499
• Suzaku-WAM, Konus-Wind, and Swift-BAT Observations of Prompt Emission of the High-Redshift GRB 050904　　　　　　　　　　　　　　　
  Satoshi Sugita; Kazutaka Yamaoka; Masanori Ohno; Makoto S. Tashiro; Yujin E. Nakagawa; Yuji Urata; Valentin Pal'shin; Sergei Golenetskii; Takanori Sakamoto; Jay Cummings; Hans Krimm; Michael Stamatikos; Ann Parsons; Scott Barthelmy; Neil Gehrels
  PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN, Volume：61, Number：3, First page：521, Last page：527, Jun. 2009, [Reviewed]
  We present the results of the high-redshift GRB 050904 at z = 6.295 from joint spectral analysis among Swift-BAT, Konus-Wind, and Suzaku-WAM, covering a wide energy range of 15-5000 keV. The nu F-nu spectrum peak energy, E-peak, was measured at 314(-89)(+173) keV, corresponding to 2291(-634)(+1263) keV in the source frame, and the isotropic equivalent radiated energy, E-iso, was estimated to be 1.04(-0.17)(+0.21) x 10(54)erg. Both are among the highest values that have ever been measured. GRBs with such a high E-iso (similar to 10(54) erg) might be associated with prompt optical emission. The derived spectral and energetic parameters are consistent with the correlation between the rest-frame E-p,E-i and the E-iso (Amati relation), but not with the correlation between the intrinsic peak energy E-p,E-i and the collimation-corrected energy E-gamma (Ghirlanda relation), unless the density of the circumburst environment of this burst is much larger than the nominal value, as suggested by other wavelength observations. We also discuss the possibility that this burst is an outlier in the correlation between E-p,E-i and the peak luminosity L-p (Yonetoku relation).
  OXFORD UNIV PRESS, English, Scientific journal
  DOI：https://doi.org/10.1093/pasj/61.3.521
  DOI ID：10.1093/pasj/61.3.521, ISSN：0004-6264, eISSN：2053-051X, Web of Science ID：WOS:000268368900016
• Multiwavelength observation from radio through very-high-energy γ-ray of OJ 287 during the 12-year cycle flare in 2007　　　　　　　　　　　　　　　
  Masaaki Hayashida; Giacomo Bonnoli; Antonio Stamerra; Elina Lindfors; Kari Nilsson; Masahiro Teshima; Hiromi Seta; Naoki Isobe; Makoto S. Tashiro; Koichiro Nakanishi; Mahito Sasada; Yoshito Shimajiri; Makoto Uemura
  31st International Cosmic Ray Conference, ICRC 2009, 2009
  We performed simultaneous multiwavelength observations of OJ 287 with the Nobeyama Millimeter Array for radio, the KANATA telescope and the KVA telescope for optical, the Suzaku satellite for X-ray and the MAGIC telescope for very high energy (VHE) γ-ray in 2007. The observations were conducted for a quiescent state in April and in a flaring state in November-December. We clearly observed increase of fluxes from radio to X-ray bands during the flaring state while MAGIC could not detect significant VHE γ-ray emission from the source. We could derive an upper limit (95% confidence level) of 1.7% of the Crab Nebula flux above 150 GeV from about 41.2 hours of the MAGIC observation. A simple SSC model suggests that the observed flaring activity could be caused by evolutions in the distribution of the electron population rather than changes of the magnetic field strength or Doppler beaming factor in the jet.
  University of Lodz, English, International conference proceedings
  SCOPUS ID：84899127842
• Design and In-Orbit Performance of the Suzaku Wide-Band All-Sky Monitor　　　　　　　　　　　　　　　
  Kazutaka Yamaoka; Akira Endo; Teruaki Enoto; Yasushi Fukazawa; Ryuji Hara; Yoshitaka Hanabata; Soojing Hong; Tsuneyoshi Kamae; Chie Kira; Natsuki Kodaka; Motohide Kokubun; Shouta Maeno; Kazuo Makishima; Ryohei Miyawaki; Kouichi Morigami; Toshio Murakami; Yujin E. Nakagawa; Kazuhiro Nakazawa; Norisuke Ohmori; Masanori Ohno; Kaori Onda; Goro Sato; Eri Sonoda; Satoshi Sugita; Masanobu Suzuki; Motoko Suzuki; Hiroyasu Tajima; Tadayuki Takahashi; Takuya Takahashi; Hiroki Tanaka; Tohru Tamagawa; Makoto S. Tashiro; Yukikatsu Terada; Takeshi Uehara; Yuji Urata; Makoto Yamauchi; Atsumasa Yoshida; Kevin Hurley; Valentin PaL'Shin; Takanori Sakamoto; Jay Cummings
  PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN, Volume：61, First page：S35, Last page：S53, Jan. 2009, [Reviewed]
  The Suzaku Wide-band All-sky Monitor (WAM) consists of thick BGO anti-coincidence shields of the Hard X-ray Detectors (HXD). It views about half of the sky and has a geometrical area of 800 cm(2) per side and an effective area of 400 cm(2), even at 1 MeV. Hence, the WAM can provide unique opportunities to detect high-energy emission from GRBs and solar flares in the sub-MeV to MeV range. The WAM has detected more than 400 GRBs and 100 solar flares since its launch. This paper describes the in-flight performance of the HXD/WAM during the initial two years of operations, including the in-flight energy response, spectral and timing capabilities, and in-orbit background.
  OXFORD UNIV PRESS, English, Scientific journal
  DOI：https://doi.org/10.1093/pasj/61.sp1.S35
  DOI ID：10.1093/pasj/61.sp1.S35, ISSN：0004-6264, eISSN：2053-051X, Web of Science ID：WOS:000264418100004
• Swift GRB GRB071010B: Outlier of the Esrcpeak - Eγ and Eiso - Esrcpeak - tsrcjet correlations　　　　　　　　　　　　　　　
  Yuji Urata; Kuiyun Huang; Myungshin Im; Induk Lee; Jinsong Deng; Winghuen Ip; Hans Krimm; Xin Liping; Masanori Ohno; Yulei Qiu; Satoshi Sugita; Makoto Tashiro; Jianyan Wei; Kazutaka Yamaoka; Weikang Zheng
  Astrophysical Journal, Volume：706, Number：1, First page：L183, Last page：L187, 2009, [Reviewed]
  We present multi-band results for GRB071010B based on Swift, Suzaku, and ground-based optical observations. This burst is an ideal target to evaluate the robustness of the Esrcpeak - Eiso and E srcpeak - Eγ relations, whose studies have been in stagnation due to the lack of the combined estimation of E srcpeak and long-term optical monitoring. The joint prompt spectral fitting using Swift/Burst Alert Telescope and Suzaku/Wide-band All-sky Monitor data yielded the spectral peak energy as Esrcpeak of 86.5+6.4-6.3 keV and Eiso of 2.25 +0.19-0.16 × 1052 erg with z = 0.947. The optical afterglow light curve is well fitted by a simple power law with temporal index α = -0.60 0.02. The lower limit of temporal break in the optical light curve is 9.8 days. Our multi-wavelength analysis reveals that GRB071010B follows Esrcpeak - Eiso but violates the Esrcpeak - Eγ and Eiso - Esrcpeak - tsrcjet at more than the 3σ level.
  Institute of Physics Publishing, English, Scientific journal
  DOI：https://doi.org/10.1088/0004-637X/706/1/L183
  DOI ID：10.1088/0004-637X/706/1/L183, ISSN：1538-4357, SCOPUS ID：77749311540
• The status and future of the third interplanetary network　　　　　　　　　　　　　　　
  K. Hurley; T. Cline; I. G. Mitrofanov; D. Golovin; M. L. Litvak; A. B. Sanin; W. Boynton; C. Fellows; K. Harshman; R. Starr; S. Golenetskii; R. Aptekar; E. Mazets; V. Pal'shin; D. Frederiks; D. M. Smith; C. Wigger; W. Hajdas; A. Zehnder; A. Von Kienlin; G. G. Lichti; A. Rau; K. Yamaoka; M. Ohno; Y. Fukazawa; T. Takahashi; M. Tashiro; Y. Terada; T. Murakami; K. Makishima; S. Barthelmy; J. Cummings; N. Gehrels; H. Krimm; J. Goldsten; E. Del Monte; M. Feroci; M. Marisaldi
  AIP Conference Proceedings, Volume：1133, First page：55, Last page：57, 2009, [Reviewed]
  The 3rd interplanetary network (IPN), which has been in operation since 1990, presently consists of 9 spacecraft: AGILE, RHESSI, Suzaku, and Swift, in low Earth orbit
  INTEGRAL, in eccentric Earth orbit with apogee 0.5 light-seconds
  Wind, up to ∼7 light-seconds from Earth
  MESSENGER, en route to Mercury
  and Mars Odyssey, in orbit around Mars. Ulysses and HETE have ceased operations, and the Fermi GBM is being incorporated into the network. The IPN operates as a full-time, all-sky monitor for transients down to a threshold of about 6x10-7 erg cm-2 or 1 photon cm-2 s -1. It detects about 275 cosmic gamma-ray bursts per year. These events are generally not the same ones detected by narrower field of view imaging instruments such as Swift, INTEGRAL IBIS, and SuperAGILE
  the localization accuracy is in the several arcminute and above range. © 2009 American Institute of Physics.
  English, International conference proceedings
  DOI：https://doi.org/10.1063/1.3155966
  DOI ID：10.1063/1.3155966, ISSN：0094-243X, SCOPUS ID：70450181998
• Reviewing Epeak relations with Swift and Suzaku data　　　　　　　　　　　　　　　
  Hans A. Krimm; Kazutaka Yamaoka; Masanori Ohno; Takanori Sakamoto; Goro Sato; Satoshi Sugita; Makoto Tashiro; R. Hara; H. Tanaka; M. Ohmori; M. Yamauchi; Kaori Onda
  AIP Conference Proceedings, Volume：1133, First page：344, Last page：349, 2009, [Reviewed]
  In recent years several authors have derived correlations between gamma-ray burst (GRB) spectral peak energy (Epeak) and either isotropic-equivalent radiated energy (Eiso) or peak luminosity (Liso). Since these relationships are controversial, but could provide redshift estimators, it is important to determine whether bursts detected by Swift exhibit the same correlations. Swift has greatly added to the number of GRBs for which redshifts are known and hence Eiso and Liso could be calculated. However, for most bursts it is not possible to adequately constrain Epeak with Swift data alone since many GRBs have Epeak above the energy range (15-150 keV) of the Swift Burst Alert Telescope (BAT). Therefore we have analyzed the spectra of 78 bursts (31 with redshift) which were detected by both Swift/BAT and the Suzaku Wide-band All-sky Monitor (WAM), which covers the energy range 50-5000 keV. For most bursts in this sample we can precisely determine Epeak and for bursts with known redshift we can compare how the Epeak relations for the Swift/Suzaku sample compare to earlier published results. © 2009 American Institute of Physics.
  English, International conference proceedings
  DOI：https://doi.org/10.1063/1.3155915
  DOI ID：10.1063/1.3155915, ISSN：0094-243X, SCOPUS ID：70450173325
• Current status of the Suzaku Wide-band All-sky Monitor (WAM)
  Yamaoka K; Sugita S; Tashiro M; Terada Y; Urata Y; Endo A; Onda K; Morigami K; Kodaka N; Sugasawara T; Iwakiri W; Fukazawa Y; Uehara T; Kira C; Hanabata Y; Yamauchi M; Sonoda E; Tanaka H; Haia R; Ohmori N; Hayashi H; Kcrno K; Hong S; Makishima K; Nakazawa K; Enoto T; Tajima H; Takahashi T; Kokubun M; Ohno M; Nakagawa Y.E; Tamagawa T; Murakami T; Hurley K
  AIP Conference Proceedings, Volume：1133, First page：91, Last page：93, 2009, [Reviewed]
  DOI：https://doi.org/10.1063/1.3155980
  DOI ID：10.1063/1.3155980, ORCID：34407210, SCOPUS ID：70450199156
• Modeling and reproducibility of suzaku HXD PIN/GSO background
  Fukazawa Y; Mizuno T; Watanabe S; Kokubun M; Takahashi H; Kawano N; Nishino S; Sasada M; Shirai H; Takahashi T; Umeki Y; Yamasaki T; Yasuda T; Bamba A; Ohno M; Takahashi T; Ushio M; Enoto T; Kitaguchi T; Makishima K; Nakazawa K; Uehara Y; Yamada S; Yuasa T; Isobe N; Kawaharada M; Tanaka T; Tashiro M.S; Terada Y; Yamaoka K
  Publications of the Astronomical Society of Japan, Volume：61, Number：SUPPL. 1, 2009, [Reviewed]
  Suzaku Hard X-ray Detector (HXD) achieved the lowest background level than any other previously or currently operational missions sensitive in the energy range of 10-600 keV, by utilizing PIN photodiodes and GSO scintillators mounted in BGO active shields to reject particle background and Compton-scattered events as much as possible. Because it does not have an imaging capability nor rocking mode for the background monitor, the sensitivity is limited by the reproducibility of the non X-ray background (NXB) model. We modeled the HXD NXB, which varies with time as well as other satellites with a low-Earth orbit, by utilizing several parameters, including particle monitor counts and satellite orbital/attitude information. The model background is supplied as an event file in which the background events are generated by random numbers, and can be analyzed in the same way as the real data. The reproducibility of the NXB model depends on the event selection criteria (such as cut-off rigidity and energy band) and the integration time, and the 1 σ systematic error is estimated to be less than 3% (PIN 15-40keV) and 1% (GSO 50-100 keV) for more than 10 ks exposure. © 2009. Astronomical Society ot Japan.
  Scientific journal
  DOI：https://doi.org/10.1093/pasj/61.sp1.s17
  Scopus Citedby：https://www.scopus.com/inward/citedby.uri?partnerID=HzOxMe3b&scp=65349126327&origin=inward
  DOI ID：10.1093/pasj/61.sp1.s17, ISSN：0004-6264, ORCID：34407120, SCOPUS ID：65349126327
• Suzaku and Multi-Wavelength Observations of OJ 287 during the Periodic Optical Outburst in 2007　　　　　　　　　　　　　　　
  Seta, Hiromi; Isobe, Naoki; Tashiro; Makoto S; Yaji, Yuichi; Arai, Akira; Fukuhara, Masayuki; Kohno, Kotaro; Nakanishi, Kouichiro; Sasada, Mahito; Shimajiri; Yoshito
  PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN, Volume：61, Number：5, First page：1011, Last page：1022, 2009, [Reviewed]
  Suzaku observations of the blazar OJ 287 were performed in 2007 April 10-13 and November 7-9. They correspond to a quiescent and a flaring state, respectively. The X-ray spectra of the source can be well-described with single power-law models in both exposures. The derived X-ray photon index and the flux density at 1 keV were found to be Gamma = 1.65 +/- 0.02 and S(1) (keV) = 215 +/- 5 nJy in the quiescent state. In the flaring state, the source exhibited a harder X-ray spectrum (Gamma = 1.50 +/- 0.01) with a nearly doubled X-ray flux density of S(1 keV) = 404(-5)(+6) nJy Moreover, significant hard X-ray signals were detected up to similar to 27 keV. In cooperation with Suzaku, simultaneous radio, optical, and very-high-energy gamma-ray observations of OJ 287 were performed with the Nobeyama Millimeter Array, the KANATA telescope, and the MAGIC telescope, respectively. The radio and optical fluxes in the flaring state (3.04 +/- 0.46 Jy and 8.93 +/- 0.05 mJy at 86.75 Hz and in the V-band, respectively) were found to be higher by a factor of 2-3 than those in the quiescent state (1.73 +/- 0.26 Jy and 3.03 +/- 0.01 mJy at 86.75 Hz and in the V-band, respectively). No notable gamma-ray
  ASTRONOMICAL SOC JAPAN, English, Scientific journal
  ISSN：0004-6264, CiNii Articles ID：10025601489, CiNii Books ID：AA1082896X
• The X-ray microcalorimeter on the NeXT mission
  Kazuhisa Mitsuda; Noriko Y. Yamasaki; Keisuke Shinozaki; Yoh Takei; Takao Nakagawai; Hiroyuki Sugitai; Yohichi Satoh; Ryuichi Fujimoto; Takaya Ohashi; Yoshitaka Ishisaki; Yuichiro Ezoe; Masahide Murakami; Makoto Tashiro; Yukikatsu Terada; Shunji Kitamoto; Toru Tamagawa; Madoka Kawaharada; Tatehiro Mihara; Richard L. Kelley; Caroline A. Kilbourne; F. Scott Porter; Peter J. Shirron; Michael J. Dipirro; Dan Mccammon; Jan Willem Den Herder
  Proceedings of SPIE - The International Society for Optical Engineering, Volume：7011, Dec. 2008
  The Soft X-ray Spectrometer (SXS) onboard the NeXT (New exploration X-ray Telescope) is an X-ray spectrometer utilizing an X-ray microcalorimeter array. Combined with the soft X-ray telescope of 6 m focal length, the instrument will have a ∼ 290cm2 effective at 6.7 keV. With the large effective area and the energy resolution as good as 6 eV (FWHM), the instrument is very suited for the high-resolution spectroscopy of iron K emission line. One of the major scientific objectives of SXS is to determine turbulent and/or macroscopic motions of the hot gas in clusters of galaxies of up to z ∼ 1. The instruments will use 6 × 6 or 8 × 8 format microcalorimeter array which is similar to that of Suzaku XRS. The detector will be cooled to a cryogenic temperature of 50 mK by multi-stage cooling system consisting of adiabatic demagnetization refrigerator, super fluid He, a 3He Joule Thomson cooler, and double-stage Stirling cycle cooler.
  DOI：https://doi.org/10.1117/12.787952
  DOI ID：10.1117/12.787952, ISSN：0277-786X, SCOPUS ID：67649225645
• Suzaku-WAM soft gamma-ray all-sky monitor by the earth occultation technique　　　　　　　　　　　　　　　
  Chie Kira; Yasushi Fukazawa; Tetsuya Asano; Hiromitsu Takahashi; Takuya Takahashi; Takeshi Uehara; Yoshitaka Hanabata; Kazutaka Yamaoka; Makoto Tashiro; Yukikatsu Terada; Masanori Ohno
  Proceedings of Science, 2008
  Suzaku Wide-band All-sky Monitor (WAM), which is the BGO Active Shield surrounding the Hard X-ray Detector (HXD) on-board Suzaku, has detected many gamma-ray bursts, soft gamma-ray repeaters, and solar flares. In addition, thanks to its large field of view (2π str), WAM can monitor bright soft gamma-ray sources with the earth occultation technique, as CGRO/BATSE. We have constructed the analysis system of the WAM earth occultation, calibrated the obtained spectra and flux by the Crab nebula, and found that the response uncertainty is around 20%. Therefore, WAM is an important all-sky monitor in the unique 50 keV - 1 MeV band against RXTE/ASM (1-10 keV) and Swift/BAT (10-100 keV), and enables us to monitor objects in wide energy band from 1 keV to 700 keV by utilizing these three instruments, as well as INTEGRAL. This is a great advantage to observe the hard tail of black hole binaries and search non-thermal components and 511 keV lines associated with the jet ejection. Here, we introduce preliminary results on Galactic black hole binaries. The long-term light curve of Cyg X-1 is successfully obtained around 100-600 keV with WAM. Together with light curves of RXTE/ASM and Swift/BAT, we can clearly see the different behavior between them. Noticeably, the bright phase in 2006 September is coincident with a detection at 0.1-1 TeV energies by MAGIC telescope. This event was also reported by RXTE/ASM, Swift/BAT and INTEGRAL/IBIS and SPI. In the average spectrum up to 700 keV of Cyg X-1, high energy cut-off is clearly seen. Furthermore, we obtained a monthly light curve and spectrum of GRS 1915+105, GX 339-4 and average spectra of some X-ray binaries. Many gamma-ray flares from black hole binaries are expected to be found by Fermi, and simultaneous X-ray monitoring with RXTE, Swift, INTEGRAL, and Suzaku is very important to constrain the emission mechanism.
  English, International conference proceedings
  ISSN：1824-8039, SCOPUS ID：84883630708
• The NeXT mission　　　　　　　　　　　　　　　
  Tadayuki Takahashi; Richard Kelley; Kazuhisa Mitsuda; Hideyo Kunleda; Robert Petre; Nicholas White; Tadayasu Dotani; Ryuichi Fujimoto; Yasushi Fukazawa; Kiyoshi Hayashida; Manabu Ishida; Yoshitaka Ishisaki; Motohide Kokubun; Kazuo Makishima; Katsuji Koyama; Greg M. Madejski; Koji Mori; Richard Mushotzky; Kazuhiro Nakazawa; Yasushi Ogasaka; Takaya Ohashi; Masanobu Ozaki; Hiroyasu Tajima; Makoto Tashiro; Yukikatsu Terada; Hiroshi Tsunemi; Takeshi Go Tsuru; Yoshihiro Ueda; Noriko Yamasaki; Shin Watanabe
  SPACE TELESCOPES AND INSTRUMENTATION 2008: ULTRAVIOLET TO GAMMA RAY, PTS 1 AND 2, Volume：7011, 2008, [Reviewed]
  The NeXT (New exploration X-ray Telescope). the new Japanese X-ray Astronomy Satellite following Suzaku, is all international X-ray mission which is currently planed for launch in 2013. NeXT is a combination of wide band X-ray spectroscopy (3-80 keV) provided by multi-layer coating, focusing hard X-ray mirror and hard X-ray imaging detectors, and high energy-resolution soft X-ray spectroscopy (0.3-10 keV) provided by thin-foil X-ray optics and a micro-calorimeter array. The mission will also carry an X-ray CCD camera as a focal plane detector for a soft, X-ray telescope and a non-focusing soft, gamma-ray detector. With these instruments, NeXT Covers very wide energy range from 0.3 keV to 600 keV. The micro-calorimeter system will be developed by international collaboration lead ISAS/JAXA and NASA. The simultaneous broad bandpass, coupled with high spectral resolution of Delta E similar to 7 eV by the micro-calorimeter will enable a wide variety of important, science themes to be pursued.
  SPIE-INT SOC OPTICAL ENGINEERING, English, International conference proceedings
  DOI：https://doi.org/10.1117/12.789640
  DOI ID：10.1117/12.789640, ISSN：0277-786X, Web of Science ID：WOS:000259563700017
• Improvement of widget　　　　　　　　　　　　　　　
  N. Kodaka; M. S. Tashiro; Y. Urata; K. Onda; W. Iwakiri; T. Sugasahara; T. Tamagawa; M. Kuwahara; S. Kageyama; F. Usui; Y. Nakada; T. Miyata; T. Aoki; T. Soyano; K. Tarusawa; H. Mito; H. Tomita
  AIP Conference Proceedings, Volume：1000, First page：559, Last page：562, 2008, [Reviewed]
  The Wide-Field Telescope for Gamma-ray burst (GRB) Early Timing (WIDGET) is a robotic telescope aiming to observe the optical emission associated with the GRB. The system has a 64°×64° wide field-of-view and tracks the Swift/BAT field-of-view automatically. The WIDGET had been operated at Akeno campus of the Institute for Cosmic Ray Research of the University of Tokyo through May 2004 to October 2006, and has been moved to Kiso observatory, IoA, University of Tokyo. For two years in Akeno, the WIDGET succeeded to observe the GRB position seven times simultaneously with the HETE2 or Swift. Based on the successful operation in Akeno, we have moved and improved the system to Kiso observatory to realize more sensitive and efficient observation. These major improvements have been carried out until March 2007 and we have succeeded to reduce the background and achieved the limiting magnitude of Mv=11-12 after color correction. © 2008 American Institute of Physics.
  English, International conference proceedings
  DOI：https://doi.org/10.1063/1.2943531
  DOI ID：10.1063/1.2943531, ISSN：0094-243X, SCOPUS ID：84874883518
• Hard X-ray Imager (HXI) for the NeXT mission　　　　　　　　　　　　　　　
  Motohide Kokubun; Kazuhiro Nakazawa; Shin Watanabe; Yasushi Fukazawa; Jun Kataoka; Hideaki Katagiri; Tsunefumi Mizuno; Kazuo Makishima; Masanori Ohno; Goro Sato; Rie Sato; Hiroyasu Tajima; Tadayuki Takahashi; Toru Tamagawa; Takaaki Ta Na Ka; Makoto Tashiro; Hiromitsu Takahashi; Yukikatsu Terada; Yasunobu Uchiyama; Yuji Urata; Kazutaka Yamaoka; Shin'ichiro Takeda; Tetsuichi Kishishita; Masayoshi Ushio; Jun'ichiro Katsuta; Shin'nosuke Ishikawa; Hirokazu Odaka; Hiroyuki Aono; Souichiro Sugimoto; Yuu Koseki; Takao Kitaguchi; Teruaki Enoto; Shin'ya Yamada; Takayuki Yuasa; Tsuyoshi Ueda; Yuichi Uehara; Sho Okuyama; Hajimu Yasuda; Sho Nishino; Yudai Umeki; Katsuhiro Hayashi; Masayuki Matsuoka; Yuki Ikejiri; Akira Endo; Yuichi Yaji; Natsuki Kodaka; Wataru Iwakiri; Tomomi Kouzu; Takako Sugasawara; Atsushi Harayama; Satoshi Nakahira
  Proceedings of SPIE - The International Society for Optical Engineering, Volume：7011, 2008
  The Hard X-ray Imager (HXI) is one of three focal plane detectors on board the NeXT (New exploration X-ray Telescope) mission, which is scheduled to be launched in 2013. By use of the hybrid structure composed of double-sided silicon strip detectors and a cadmium telluride strip detector, it fully covers the energy range of photons collected with the hard X-ray telescope up to 80 keV with a high quantum efficiency. High spatial resolutions of 400 micron pitch and energy resolutions of 1-2 keV (FWMH) are at the same time achieved with low noise front-end ASICs. In addition, thick BGO active shields compactly surrounding the main detection part, as a heritage of the successful performance of the Hard X-ray Detector (HXD) on board Suzaku satellite, enable to achive an extremely high background reduction for the cosmic-ray particle background and in-orbit activation. The current status of hardware development including the design requirement, expected performance, and technical readinesses of key technologies are summarized.
  International conference proceedings
  DOI：https://doi.org/10.1117/12.788290
  Scopus：https://www.scopus.com/inward/record.uri?partnerID=HzOxMe3b&scp=67649215322&origin=inward
  Scopus Citedby：https://www.scopus.com/inward/citedby.uri?partnerID=HzOxMe3b&scp=67649215322&origin=inward
  DOI ID：10.1117/12.788290, ISSN：0277-786X, SCOPUS ID：67649215322
• Correlative Analysis of GRBs detected by Swift and Suzaku-WAM　　　　　　　　　　　　　　　
  Hans Krimm; Kazutaka Yamaoka; Masanori Ohno; Makoto Tashiro; Kaori Onda; Goro Sato; Takanori Sakamoto; Satoshi Sugita
  AIP Conference Proceedings, Volume：1000, First page：129, Last page：132, 2008, [Reviewed]
  Since most gamma-ray bursts (GRBs) have a peak energy (Epeak) above the energy range (15-150 keV) of the Burst Alert Telescope (BAT) on Swift, a full understanding of the prompt emission from Swift GRBs requires spectral fits over as broad an energy range as possible. This can be done for bursts which are simultaneously detected by Swift BAT and the Suzaku Wide-band All-Sky Monitor (WAM), which covers the energy range from 50-5000 keV. Since the launch of Suzaku in July 2005, there have been 33 gamma-ray bursts (GRBs) which have triggered both Swift and WAM. A joint BAT-WAM team has cross-calibrated the two instruments using GRBs, and we are now able to perform joint fits on these bursts to determine spectral parameters including Epeak. The results of broad spectral fits allows us to understand the distribution of Epeak for Swift bursts and to calibrate Epeak estimators when Epeak is within the BAT energy range. For those bursts with spectroscopic redshifts, we can calculate the isotropic energy and study various correlations between Epeak and other global burst parameters. Here we present preliminary results of joint Swift/BAT-Suzaku/WAM spectral fits. © 2008 American Institute of Physics.
  English, International conference proceedings
  DOI：https://doi.org/10.1063/1.2943426
  DOI ID：10.1063/1.2943426, ISSN：0094-243X, SCOPUS ID：84874922105
• Suzaku-WAM, Konus-Wind, and Swift-BAT observations of the prompt emission of the highest redshift GRB 050904　　　　　　　　　　　　　　　
  Satoshi Sugita; Kazutaka Yamaoka; Masanori Ohno; Makoto Tashiro; Valentin Pal'Shin; Sergei Golenetskii; Takanori Sakamoto; Jay Cummings; Hans Krimm; Michael Stamatikos; Ann Parsons; Scott Barthelmy; Neil Gehrels
  AIP Conference Proceedings, Volume：1000, First page：354, Last page：357, 2008, [Reviewed]
  We present the results of the highest redshift GRB 050904 from joint spectral analyses among Swift/BAT, Konus-Wind and Suzaku-WAM covering a wide energy range of 15-5000 keV. The peak energy was first measured at 338 -93 +168keV, corresponding to 2465-678 +1225keV in the source frame. This is one of the highest value that has been ever meaured. The derived spectral and energetic parameters are consisitent with the Amati relation, but not with the Ghirlada relation. This implies that the circumburst density of this burst might be larger than the nominal value, as suggested by other wavelength observations. We also found that the burst could be an outlier in Yonetoku relation. © 2008 American Institute of Physics.
  English, International conference proceedings
  DOI：https://doi.org/10.1063/1.2943482
  DOI ID：10.1063/1.2943482, ISSN：0094-243X, SCOPUS ID：84857873900
• Design of the two-stage series adiabatic demagnetization refrigerator for the NeXT and Spectrum-RG missions　　　　　　　　　　　　　　　
  K. Shinozaki; K. Mitsuda; N. Y. Yamasaki; Y. Takei; M. DiPirro; Y. Ezoe; R. Fujimoto; J. W. den Herder; M. Hirabayashi; Y. Ishisaki; K. Kanao; M. Kawaharada; R. Kelley; C. Kilbourne; S. Kitamoto; D. McCammon; T. Mihara; M. Murakami; T. Nakagawa; T. Ohashi; F. S. Porter; Y. Satoh; P. Shirron; H. Sugita; T. Tamagawa; M. Tashiro; S. Yoshida
  SPACE TELESCOPES AND INSTRUMENTATION 2008: ULTRAVIOLET TO GAMMA RAY, PTS 1 AND 2, Volume：7011, 2008, [Reviewed]
  The SXS (Soft X-ray Spectrometer) onboard the coming Japanese X-ray satellite NeXT (New Exploration Xray Telescope) and the SXC (Spectrum-RC X-ray Calorimeter) in Spectrum-RG mission are microcalorimeter array spectrometers which will achieve high spectral resolution of similar to 6 eV in 0.3-10.0 keV energy band. These spectrometers are well-suited to address key problems in high-energy astrophysics. To achieve these high spectral sensitivities, these detectors require to be operated under 50 mK by using very efficient cooling systems including adiabatic demagnetization refrigerator (ADR,). For both missions, we propose a two-stage series ADR as a cooling system below 1 K, in which two units of ADR consists of magnetic cooling material, a superconducting magnet, and a heat switch are operated step by step. Three designs of the ADR are proposed for SXS/SXC. In all three designs, ADR can attain the required hold time of 23 hours at 50 mK and cooling power of 0.4 mu W with a low magnetic fields (1.5/1.5 Tesla or 2.0/3.0 Tesla) in a small configuration (180 mm phi x 319 mm in length).
  We also fabricated a new portable refrigerator for a, technology investigation of two-stage ADR. Two units of ADR have been installed at the bottom of liquid He tank. By using this dewar, important technologies such as an operation of two-stage cooling cycle, tight temperature control less than 1 mu K (in rms) stability, a, magnetic shielding, saltpills, and gas-gap heat switches are evaluated.
  SPIE-INT SOC OPTICAL ENGINEERING, English, International conference proceedings
  DOI：https://doi.org/10.1117/12.788634
  DOI ID：10.1117/12.788634, ISSN：0277-786X, Web of Science ID：WOS:000259563700109
• Investigation of jet break features in Swift gamma-ray bursts
  Sato G; Yamazaki R; Ioka K; Sakamoto T; Takahashi T; Nakazawa K; Nakamura T; Toma K; Hullinger D; Tashiro M; Parsons A.M; Krimm H.A; Barthelmy S.D; Gehrels N; Burrows D.N; O{'}Brien P.T; Osborne J.P; Chincarini G; Lamb D.Q
  11th Marcel Grossmann Meeting on Recent Developments in Theoretical and Experimental General Relativity, Gravitation and Relativistic Field Theories - Proc. of the MG11 Meeting on General Relativity, First page：2033, Last page：2035, 2008, [Reviewed]
  ORCID：34141392, SCOPUS ID：84892974067
• Status of GRB observations with the suzaku wideband all-sky monitor
  Tashiro M.S; Terada Y; Urata Y; Onda K; Kodaka N; Endo A; Suzuki M; Morigami K; Yamaoka K; Nakagawa Y.E; Sugita S; Fukazawa Y; Ohno M; Takahashi T; Kira C; Uehara T; Tamagawa T; Enoto T; Miyawaki R; Nakazawa K; Makishima K; Sonoda E; Yamauchi M; Maeno S; Tanaka H; Hara R; Suzuki M; Kokubun M; Takahashi T; Hong S.J; Murakami T; Tajima H
  AIP Conference Proceedings, Volume：1000, First page：162, Last page：165, 2008, [Reviewed]
  DOI：https://doi.org/10.1063/1.2943434
  DOI ID：10.1063/1.2943434, ORCID：34407145, SCOPUS ID：84874885942
• Suzaku HXD-WAM observations of gamma-ray prompt emission and collaboration with GLAST
  Fukazawa Y; Ohno M; Takahashi T; Asano T; Uehara T; Yamaoka K; Sugita S; Terada Y; Tamagawa T; Suzuki M; Tashiro M; Urata Y; Abe K; Onda K; Suzuki M; Sonoda E; Sato G; Enoto T; Makishima K; Takahashi T; Kokubun M; Nakazawa K
  AIP Conference Proceedings, Volume：921, First page：106, Last page：108, 2007, [Reviewed]
  DOI：https://doi.org/10.1063/1.2757279
  DOI ID：10.1063/1.2757279, ORCID：34407196, SCOPUS ID：77957868982
• The Suzaku-Swift joint observation of the early X-ray afterglow of GRB060105　　　　　　　　　　　　　　　
  Makoto S. Tashiro; Keiichi Abe; Lorella Angelini; Scott Barthelmy; Neil Gehrels; Nobuyuki Ishikawa; Louis J. Kaluzienski; Nobuyuki Kawai; Richard L. Kelley; Kenzo Kinugasa; Hironobu Kodaira; Takayoshi Kohmura; Kaori Kubota; Yoshitomo Maeda; Shouta Maeno; Hiroshi Murakami; Toshio Murakami; Yujin E. Nakagawa; Kazuhiro Nakazawa; John Nousek; Shin'ya Okuno; Kaori Onda; James N. Reeves; George Ricker; Goro Sato; Eri Sonoda; Motoko Suzuki; Tadayuki Takahashi; Toru Tamagawa; Ken'ichi Torii; Yoshihiro Ueda; Yuji Urata; Kazutaka Yamaoka; Makoto Yamauchi; Daisuke Yonetoku; Atsumasa Yoshida; Satoru Yoshinari
  PROGRESS OF THEORETICAL PHYSICS SUPPLEMENT, Number：169, First page：3, Last page：6, 2007, [Reviewed]
  Results are presented of a Suzaku and Swift joint observation for an early X-ray afterglow of GRB 060105. The bright, long gamma-ray burst GRB 060105 triggered the Swift Burst Alert Telescope (BAT) at 06:49:28 on 5 January 2006 (To). The Suzaku team commenced a pre-planned target of opportunity observation at 12:10 and continued till 12:00 on January 6. The X-ray flux faded during the observations from 6.8 x 10(-9) erg s(-1)cm(-2) to 1.5 x 10(-13) erg s(-1)cm(-2) in the 2-10 keV energy band. Following the prompt emission and successive "very steep decay", a "shallow decay" was observed from T-0 + 187 s to T-0 + 1287 s. After an observation gap during T-0 + (1.5 - 3) ks, an extremely early steep decay was observed in To + (4 - 30) ks. The steep decay exhibited decay indices of 2.3 - 2.4. This very early break, if it is a jet break, is the earliest case among X-ray afterglow observations, suggesting a very narrow jet whose opening angle is well below 1 degrees.
  PROGRESS THEORETICAL PHYSICS PUBLICATION OFFICE, English, Scientific journal
  ISSN：0375-9687, Web of Science ID：WOS:000252207900003
• Capability and strategy of the X-ray afterglow observation with Suzaku　　　　　　　　　　　　　　　
  M. S. Tashiro; T. Murakami; A. Yoshida; N. Kawai; J. Nousek; L. Angelini; J. L. Kaluzienski; L. R. Kelley; K. Kinugasa; K. Nakazawa; N. J. Reeves; G. Ricker; M. Suzuki; T. Takahashi; T. Tamagawa; K. Torii; Y. Ueda; Y. Urata; K. Yamaoka; M. Yamauchi; D. Yonetoku
  Nuovo Cimento della Societa Italiana di Fisica B, Volume：121, Number：12, First page：1597, Last page：1598, Dec. 2006
  The Japanese X-ray astronomical satellite Suzaku launched in July 2005 is equipped with two kinds of X-ray instruments for the wide-band spectroscopy. The X-ray CCD cameras (XIS) cover 0.3 to 12 keV with the energy resolution of 120 eV at 6 keV. The Hard X-ray Detector (HXD) consisting of well-type phoswitch counters covers 40-600 keV. With these instruments, we organized a team for quick follow-up observations of gamma-ray bursts, aiming to observe the afterglow phase transition and to search for spectral features with the wide band X-ray instruments. © Società Italiana di Fisica.
  English, International conference proceedings
  DOI：https://doi.org/10.1393/ncb/i2007-10323-9
  DOI ID：10.1393/ncb/i2007-10323-9, ISSN：1594-9982, SCOPUS ID：35348967905
• Detailed analyses of GRB 060105 X-ray afterglow observed by Suzaku　　　　　　　　　　　　　　　
  Y. E. Nakagawa; M. Tashiro; K. Abe; A. Yoshida; K. Yamaoka; K. Nakazawa; T. Murakami; D. Yonetoku; N. Kawai; J. Nousek; N. Ishikawa; Y. Urata; K. Onda; T. Tamagawa; M. Suzuki; M. Kuwahara; T. Takahashi; M. Yamauchi; E. Sonoda; S. Maeno; K. Kinugasa; T. Kohmura; K. Torii; Y. Ueda; K. Kubota; K. Sugiyasu; H. Kodaira; S. Okuno; S. Yoshinari; T. Shimokawabe; T. Ishimura; G. R. Ricker; J. N. Reeves; L. Angelini; L. J. Kaluzienski; R. L. Kelley
  Nuovo Cimento della Societa Italiana di Fisica B, Volume：121, Number：12, First page：1531, Last page：1533, Dec. 2006, [Reviewed]
  GRB 060105 was detected with the BAT instrument on-board Swift. The Suzaku follow-up observation started just 5.3 hours after the trigger with the XIS and HXD instruments. The XIS detected an uncatalogued fading source and its position was consistent with that previously reported by Swift XRT. We performed the spectral analyses using the data derived from Suzaku XIS and Swift XRT, and found that the spectrum of X-ray afterglow was well reproduced by the absorbed power law model. The best-fit spectral index and absorption are β = 2.15 ± 0.03 and NH = (3.74 ± 0.03) × 1021 cm-2, respectively. The observed decay curve by Suzaku XIS is fully consistent with the Swift XRT result. The Suzaku and Swift observations imply the possibility of the jet break at t = 3500 s, and the brightening of afterglow around t = 40000 s likely due to the refreshed shock. We see neither significant spectral evolution during the decay, nor evidence of emission line feature. © Società Italiana di Fisica.
  English, International conference proceedings
  DOI：https://doi.org/10.1393/ncb/i2007-10316-8
  DOI ID：10.1393/ncb/i2007-10316-8, ISSN：1594-9982, SCOPUS ID：35349011131
• Optical shallow decay and re-brightening phase of early afterglow　　　　　　　　　　　　　　　
  Y. Urata; K. Y. Huang; W. H. Ip; J. Hu; Y. Qiu; P. H. Kuo; Y. H. Li; T. Tamagawa; M. Tashiro; K. Onda; K. Abe; K. Ioka; M. Kuwahara; W. K. Zheng; M. Zhai; J. Y. Wei; J. S. Deng; N. Kodaka; K. Masuno
  NUOVO CIMENTO DELLA SOCIETA ITALIANA DI FISICA B-BASIC TOPICS IN PHYSICS, Volume：121, Number：12, First page：1601, Last page：1603, Dec. 2006, [Reviewed]
  Utilizing East Asian GRB Follow-up Observation Network (EAFON), we have obtained 3 major results; 1) first long-term monitoring of short GRB afterglow from similar to 0.1 days after the burst, 2) multi band monitoring of early optical shallow decay and re-brightening phase, 3) catch about 30 high-redshift GRB candidates. In this paper, we present shallow decay phase and re-brightening phase of early optical afterglow. Our results imply that these phases are unlikely to be caused by the variable external density model. Overall.1 day light curve behavior may be explained by Patchy shell model and/or different emission region such as 2 jets model rather than to be described by refreshed shock scenario.
  SOC ITALIANA FISICA, English, Scientific journal
  DOI：https://doi.org/10.1393/ncb/i2007-10325-7
  DOI ID：10.1393/ncb/i2007-10325-7, ISSN：2037-4895, eISSN：1594-9982, Web of Science ID：WOS:000250546900068
• Optical afterglows detected by the lulin one-meter telescope(*)　　　　　　　　　　　　　　　
  K. Y. Huang; Y. Urata; P. H. Kuo; Y. H. Lee; W. H. Ip; T. Tamagawa; K. Onda; M. Tashiro; Y. Qiu; K. Makishima
  NUOVO CIMENTO DELLA SOCIETA ITALIANA DI FISICA B-BASIC TOPICS IN PHYSICS, Volume：121, Number：12, First page：1489, Last page：1490, Dec. 2006, [Reviewed]
  The Lulin One-meter Telescope (LOT) has started GRBs follow-up since July 2003. In total, fifteen optical afterglows were detected successfully until July 2006. In this paper, we summarize these afterglows and two of them are described in detail. The two events are 1) GRB 040924, a GRB with cooling break and 2) GRB 050319, whose multi-color light curve shows different properties compared with Swift/XRT observations.
  SOC ITALIANA FISICA, English, Scientific journal
  DOI：https://doi.org/10.1393/ncb/i2007-10290-1
  DOI ID：10.1393/ncb/i2007-10290-1, ISSN：2037-4895, eISSN：1594-9982, Web of Science ID：WOS:000250546900026
• Ultra wide-field telescope WIDGET for observing GRB(*)　　　　　　　　　　　　　　　
  K. Onda; T. Tamagawa; M. Tashiro; Y. Urata; K. Abe; M. Kuwahara; F. Usui; N. Kodaka; K. Masuno; H. Azuma
  NUOVO CIMENTO DELLA SOCIETA ITALIANA DI FISICA B-BASIC TOPICS IN PHYSICS, Volume：121, Number：12, First page：1549, Last page：1550, Dec. 2006, [Reviewed]
  The WIDe-field telescope for Gamma-ray burst in Early Timing (WIDGET) is an automated optical telescope designed to detect the expected optical prompt emission associating with the Gamma-Ray Burst (GRBs). To search for the optical prompt emissions or possible pre-cursors, the system is programmed to track the HETE-2 and Swift field of views. The WIDGET has been operated since May 2004. So far, it succeeded 15 times to observe the GRB field at the same time of HETE-2 or Swift trigger and we succeeded to obtain the upper limits for the 7 GRBs.
  SOC ITALIANA FISICA, English, Scientific journal
  DOI：https://doi.org/10.1393/ncb/i2007-10303-1
  DOI ID：10.1393/ncb/i2007-10303-1, ISSN：2037-4895, eISSN：1594-9982, Web of Science ID：WOS:000250546900050
• The electron and magnetic field energies in the east lobe of the radio galaxy Fornax A, measured with XMM-Newton　　　　　　　　　　　　　　　
  N Isobe; K Makishima; M Tashiro; K Ito; N Iyomoto; H Kaneda
  PROCEEDINGS OF THE X-RAY UNIVERSE 2005, VOLS 1 AND 2, Volume：604, First page：585, Last page：+, 2006, [Reviewed]
  In an XMM-Newton observation of the east lobe of nearby radio galaxy Fonrax A, we have significantly detected the diffuse X-ray emission, which was originally discovered by ASCA and ROSAT. The X-ray spectrum of the diffuse emission is described by a single powerlaw model, modified with the Galactic absorption toward the object. The best-fit X-ray photon index, 1.62(-0.15)(+0.25), agrees well with the synchrotron radio index, 1.68 +/- 0.05, between 29.9 MHz and 5 GHz. Therefore, the inverse Compton interpretation for the diffuse X-ray emission is justified. A comparison between the radio and Xray flux densities gives a moderate electron-energy dominance over in the east lobe of Fornax A, in spite of the dormancy of its nucleus. We also reexamined the ASCA result on the west lobe, to find that both lobes share the similar physical condition.
  ESA PUBLICATIONS DIVISION C/O ESTEC, English, International conference proceedings
  ISSN：0379-6566, Web of Science ID：WOS:000236905300154
• In Orbit Timing Calibration of the Suzaku Hard X-ray Detector　　　　　　　　　　　　　　　
  Yukikatsu Terada; Teruaki Enoto; Ryouhei Miyawaki; Yasushi Fukazawa; Madoka Kawaharada; Tsuneyoshi Kamae; Motohide Kokubun; Kazuo Makishima; Tsunefumi Mizuno; Toshio Murakami; Kazuhiro Nakazawa; Masaharu Nomach; Tadayuki Takahashi; Hiromitsu Takahashi; Makoto S. Tashiro; Toru Tamagawa; Shin Watanabe; Kazutaka Yamaoka; Daisuke Yonetoku
  2006 IEEE NUCLEAR SCIENCE SYMPOSIUM CONFERENCE RECORD, VOL 1-6, Volume：2, First page：783, Last page：787, 2006, [Reviewed]
  Suzaku is the fifth Japanese astrophysical satellite, devoted to study high energy phenomena in the X-ray band of 0.5 - 600 keV. It was successfully launched from Uchinoura Space Center in Japan on 10th July 2005. The HXD on board Suzaku covers 10 - 600 keV band with a high sensitivity of about 10(-5) cnt/s/cm(2)/keV level. The sensor consists of 16 identical GSO/BGO well-type-phoswich counters incorporating 2 mm-thick silicon PIN diodes, and 20 surrounding-BGO-shield counters to remove residual non X-ray backgrounds through anti-coincidence rejection. The present paper is particularly focused on timing system of the HXD and in-orbit verifications with pulsars.
  IEEE, English, International conference proceedings
  DOI：https://doi.org/10.1109/NSSMIC.2006.355968
  DOI ID：10.1109/NSSMIC.2006.355968, ISSN：1082-3654, ORCID：34407218, SCOPUS ID：38649105205, Web of Science ID：WOS:000288875600156
• Suzaku wide-band all-sky monitor observations of GRB prompt emissions
  Yamaoka K; Sugita S; Ohno M; Takahashi T; Fukazawa Y; Terada Y; Endo Y; Hong S; Abe K; Onda K; Tashiro M; Enoto T; Miyawaki R; Kokubun M; Makishima K; Sato G; Nakazawa K; Takahashi T
  AIP Conference Proceedings, Volume：836, First page：201, Last page：204, 2006, [Reviewed]
  DOI：https://doi.org/10.1063/1.2207890
  DOI ID：10.1063/1.2207890, ORCID：34407133, SCOPUS ID：33845567323
• In-orbit performance of the Suzaku wide-band all-sky monitor - art. no. 626643　　　　　　　　　　　　　　　
  Yamaoka Kazutaka; Sugita Satoshi; Ohno Masanori; Takahashi Takuya; Fukazawa Yasushi; Terada Yukikatsu; Tamagawa Tohru; Abe Keiichi; Endo Yasuhiko; Onda Kaori; Matsumura Satoshi; Tashiro Makoto; Hong Soojing; Sato Goro; Nakazawa Kazuhiro; Takahashi Tadayuki; Miyawaki Ryohei; Enoto Teruaki; Kokubun Motohide; Makishima Kazuo; Murakami Toshio
  Space Telescopes and Instrumentation II: Ultraviolet to Gamma Ray, Pts 1 and 2, Volume：6266, First page：26643, 2006, [Reviewed]
  The X-ray astronomical satellite Suzaku was successfully launched in July 2005. The onboard Wideband All-sky Monitor (WAM) is designed as the second function of the large, thick BGO anti-coincidence shields of the Hard X-ray Detectors (HXD). It views about half of the whole sky and has a geometrical area of 800 cm(2) per side, with a large effective area of 400 cm(2) even at 1 MeV. Hence, the WAM is expected to provide unique opportunities to detect high energy emission from GRBs and solar flares in the MeV range. In fact, the WAM has detected at least 47 GRBs, although the fine-tuning of the GRB functions is still in progress. The most impressive GRB result is the bright, hard spectrum GRB 051008, which was detected up to 1 MeV with the WAM. We will present here the in-flight performance of the HXD/WAM during the initial eight-months of operations. The in-flight energy response, spectral and timing capabilities, and in-orbit background are described in this paper.
  SPIE-INT SOC OPTICAL ENGINEERING, English, International conference proceedings
  DOI：https://doi.org/10.1117/12.671994
  DOI ID：10.1117/12.671994, ISSN：0277-786X, eISSN：1996-756X, Web of Science ID：WOS:000240015400124
• Hard X-ray Imager for the NeXT Mission　　　　　　　　　　　　　　　
  Nakazawa Kazuhiro; Fukazawa Yasushi; Kamae Tuneyoshi; Kataoka Jun; Kokubun Motohide; Makishima Kazuo; Mizuno Tsunefumi; Murakami Toshio; Nomachi Masaharu; Tajima Hiroyasu; Takahashi Tadayuki; Tashiro Makoto; Tamagawa Toru; Terada Yukikatsu; Watanabe Shin; Yamaoka Kazutaka; Yonetoku Daisuke
  SPACE TELESCOPES AND INSTRUMENTATION II: ULTRAVIOLET TO GAMMA RAY, PTS 1 AND 2, Volume：6266, 2006, [Reviewed]
  The hard X-ray imager (HXI) is the primary detector of the NeXT mission, proposed to explore high-energy non-thermal phenomena in the universe. Combined with a novel hard X-ray mirror optics, the HXI is designed to provide better than arc-minutes imaging capability with 1 keV level spectroscopy, and more than 30 times higher sensitivity compared with any existing hard X-ray instruments. The base-line design of the HXI is improving to secure high sensitivity. The key is to reduce the detector background as far as possible. Based on the experience of the Suzaku satellite launched in July 2005, the current design has a well-type tight active shield and multi layered, multi material imaging detector made of Si and CdTe. Technology has been under development for a few years so that we have reached the level where a basic detector performance is satisfied. Design tuning to further improve the sensitivity and reliability is on-going.
  International conference proceedings
  DOI：https://doi.org/10.1117/12.670674
  Scopus：https://www.scopus.com/inward/record.uri?partnerID=HzOxMe3b&scp=33748993428&origin=inward
  Scopus Citedby：https://www.scopus.com/inward/citedby.uri?partnerID=HzOxMe3b&scp=33748993428&origin=inward
  DOI ID：10.1117/12.670674, ISSN：0277-786X, SCOPUS ID：33748993428, Web of Science ID：WOS:000240015400075
• Swift Left the Earth　　　　　　　　　　　　　　　
  TASHIRO Makoto
  Butsuri, Volume：60, Number：5, First page：373, Last page：376, May 2005
  The Physical Society of Japan (JPS), Japanese
  DOI：https://doi.org/10.11316/butsuri1946.60.373
  DOI ID：10.11316/butsuri1946.60.373, ISSN：0029-0181, CiNii Articles ID：110002078630, CiNii Books ID：AN00196952
• Erratum: The swift Gamma-ray burst mission (Astrophysical Journal (2004) 611: (1005))　　　　　　　　　　　　　　　
  N. Gehrels; G. Chincarini; P. Giommi; K. O. Mason; J. A. Nousek; A. A. Wells; N. E. White; S. D. Barthelmy; D. N. Burrows; L. R. Cominsky; K. C. Hurley; F. E. Marshall; P. Mészáros; P. W.A. Roming; L. Angelini; L. M. Barbier; T. Belloni; P. T. Boyd; S. Campana; P. A. Caraveo; M. M. Chester; O. Citerio; T. L. Cline; M. S. Cropper; J. R. Cumminos; A. J. Dean; E. D. Feigelson; E. E. Fenimore; D. A. Frail; A. S. Fruchter; G. P. Garmire; K. Gendreau; G. Ghisellini; J. Greiner; J. E. Hill; S. D. Hunsberger; H. A. Krimm; S. R. Kulkarni; P. Kumar; F. Lebrun; N. M. Lloyd-Ronning; C. B. Markwardt; B. J. Mattson; R. F. Mushotzky; J. P. Norris; B. Paczynski; D. M. Palmer; H. S. Park; A. M. Parsons; J. Paul; M. J. Rees; C. S. Reynolds; J. E. Rhoads; T. P. Sasseen; B. E. Schaefer; A. T. Short; A. P. Smale; I. A. Smith; L. Stella; M. Still; G. Tagliaferri; T. Takahashi; M. Tashiro; L. K. Townsley; J. Tueller; M. J.L. Turner; M. Vietri; W. Voges; M. J. Ward; R. Wlllingale; F. M. Zerbi; W. W. Zhang
  Astrophysical Journal, Volume：621, Number：1 I, First page：558, Mar. 2005
  Institute of Physics Publishing, English, Scientific journal
  DOI：https://doi.org/10.1086/427409
  DOI ID：10.1086/427409, ISSN：1538-4357, SCOPUS ID：20244373337
• The search for optical emission on and before the GRB trigger with the WIDGET telescope　　　　　　　　　　　　　　　
  T. Tamagawa; F. Usui; Y. Urata; K. Abe; K. Onda; M. Tashiro; Y. Terada; H. Fujiwara; N. Miura; S. Hirose; N. Kawai; A. Yoshida; M. Mori; K. Makishima
  Nuovo Cimento della Societa Italiana di Fisica C, Volume：28, Number：4-5, First page：771, Last page：774, 2005
  WIDGET is a robotic telescope for monitoring the HETE-2 field-of-view to detect Gamma-Ray Burst optical flashes or possible optical precursors. The system has 62° × 62° wide field-of-view which covers about 80% of HETE-2 one with a 2k×2k Apogee U10 CCD camera and a Canon EF 24 mm f/1.4 wide-angle lens without a bandpass filter. WIDGET has been in operation since June 2004 at Akeno observing site where is about 200 km apart from Tokyo. Typical limiting magnitude with S/N = 3 at the site is V = 10mag for 5 seconds exposure and V = 11mag for 30 seconds exposure. We had already six coincident observations with HETE-2 position alerts. It was, however, cloudy for all cases due to rainy season in Japan. The expected number of coincident observations under clear sky is about 5 events per year. We will extend the system in early 2005 for Swift era to monitor optical transients in wider field-of-view, multi-color or polarization modes. © Società Italiana di Fisica.
  Editrice Compositori s.r.l., English, Scientific journal
  ISSN：1826-9885, SCOPUS ID：29344451956
• Performance of GRB monitor with Astro-E2 Hard X-ray Detector (HXD-II)　　　　　　　　　　　　　　　
  S. Hong; K. Yamaoka; Y. Terada; M. Ohno; A. Tsutsui; Y. Endo; J. Kotoku; Y. Okada; M. Mori; Y. Fukazawa; T. Kamae; M. Kokubun; K. Makishima; T. Murakami; K. Nakazawa; M. Nomachi; M. Tashiro; I. Takahashi; T. Takahashi; D. Yonetoku; S. Watanabe
  Nuovo Cimento della Societa Italiana di Fisica C, Volume：28, Number：4-5, First page：821, Last page：824, 2005
  The Hard X-ray Detector (HXD-II) is one of the three instruments onboard the Astro-E2 satellite scheduled for launch in 2005. The HXD-II consists of 16 main counters (Well units), surrounded by 20 active shield counters (Anti units). The Anti units have a large geometrical area of ∼ 800 cm2 with an uncollimated field of view covering ∼ 2π steradian. Utilizing 2.6 cm thick BGO crystals, they realize a large effective area of 400 cm 2 for 1 MeV photons. In the energy range of 300-5000 keV, the expected effective area is significantly larger than those of other gamma-ray burst instruments, such as CGRO/BATSE, HETE-2/FREGATE, and GLAST/GBM. Therefore, the Anti units act as a Wideband All-sky Monitor (WAM) for gamma-ray bursts in the energy range of 50-5000 keV. © Società Italiana di Fisica.
  Scientific journal
  Scopus：https://www.scopus.com/inward/record.uri?partnerID=HzOxMe3b&scp=29344457423&origin=inward
  Scopus Citedby：https://www.scopus.com/inward/citedby.uri?partnerID=HzOxMe3b&scp=29344457423&origin=inward
  ISSN：2037-4909, eISSN：1826-9885, SCOPUS ID：29344457423
• Development of the HXD anti counters onboard Astro-E2　　　　　　　　　　　　　　　
  Kazutaka Yamaoka; Masanoria Ohno; Yukikatsu Terada; Soojing Hong; Jun'ichi Kotoku; Yu Okada; Akihito Tsutsui; Masanori Mori; Kazuo Makishima; Motohide Kokubun; Toshio Murakami; Daisuke Yonetoku; Masaharu Nomachi; Tsuneyoshi Kamae; Tadayuki Takahashi; Kazuhiro Nakazawa; Makoto Tashiro; Isao Takahashi; Shin Watanabe; Yasushi Fukazawa
  IEEE Nuclear Science Symposium Conference Record, Volume：1, First page：309, Last page：313, Dec. 2004, [Reviewed]
  The Hard X-ray Detector (HXD) is one of the three instruments onboard Japanese X-ray astronomy satellite Astro-E2 scheduled for launch in 2005. This mission is very unique in a point of having a lower detector background than any other past missions in the 10-600 keV range. In the HXD, the large and thick BGO crystal are used as active shields for reducing the particle and gamma-ray background to the main detector. These anticoincidence shields are called as "Anti counters", which have a large geometrical area ∼ 800 cm 2 and an uncollimated field of view of ∼ 2π. Furthemore, they also have a larger effective area, corresponding to 400 cm 2 at even 1 MeV due to their thick high-Z materials. This feature enables us to observe the high energy radiation of Gamma-ray bursts with a higher sensitivity than previous all-sky monitors. Hence, the Anti counters have been developed as all-sky monitors with a broadband coverage of 50-5000 keV. In this paper, we will describe overall design of the HXD Anti counters, then report on the results of the pre-flight calibration test on June 2004 using the flight model. By irradiating various radio isotopes with Anti counters, we confirmed that they have capability as all-sky monitors. It is striking that the low energy threshold has been archived about 30 keV in spite of large volume of BGO scintillators. © 2004 IEEE.
  International conference proceedings
  Scopus Citedby：https://www.scopus.com/inward/citedby.uri?partnerID=HzOxMe3b&scp=23844458303&origin=inward
  ISSN：1095-7863, SCOPUS ID：23844458303
• Improvements of the Astro-E2 Hard X-ray Detector (HXD-II)　　　　　　　　　　　　　　　
  M Kokubun; K Abe; Y Ezoe; Y Fukazawa; S Hong; H Inoue; T Itoh; T Kamae; D Kasama; M Kawaharada; N Kawano; K Kawashima; S Kawasoe; Y Kobayashi; J Kotoku; M Kouda; A Kubota; GM Madejski; K Makishima; T Mitani; H Miyasaka; R Miyawaki; K Mori; M Mori; T Murakami; MM Murashima; K Nakazawa; H Niko; M Nomachi; M Ohno; Y Okada; K Oonuki; G Sato; M Suzuki; H Takahashi; Takahashi, I; T Takahashi; K Tamura; T Tanaka; M Tashiro; Y Terada; S Tominaga; S Watanabe; K Yamaoka; T Yanagida; D Yonetoku
  IEEE TRANSACTIONS ON NUCLEAR SCIENCE, Volume：51, Number：5, First page：1991, Last page：1996, Oct. 2004, [Reviewed]
  We summarize significant improvements which have been achived in the development of Astro-E2 Hard X-ray Detector (HXD-II). An expanded energy range and better energy resolution have been achieved from progresses in device materials and redesigning of the front-end electronics. An improved estimation for the detector background in orbit has also been conducted based upon results from our proton irradiation experiment. The sensitivity of HXD-II can be expected to reach an order of 10(-6) [c s(-1) keV(-1) cm(-2)].
  IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC, English, Scientific journal
  DOI：https://doi.org/10.1109/TNS.2004.832921
  DOI ID：10.1109/TNS.2004.832921, ISSN：0018-9499, SCOPUS ID：8344229310, Web of Science ID：WOS:000224490900011
• Development of the HXD anti counters onboard Astro-E2　　　　　　　　　　　　　　　
  K Yamaoka; M Ohno; Y Terada; S Hong; J Kotoku; Y Okada; A Tsutsui; M Mori; K Makishima; M Kokubun; T Murakami; D Yonetoku; M Nomachi; T Kamae; T Takahashi; K Nakazawa; M Tashiro; Takahashi, I; S Watanabe; Y Fukazawa
  2004 IEEE Nuclear Science Symposium Conference Record, Vols 1-7, First page：309, Last page：313, 2004, [Reviewed]
  The Hard X-ray Detector (HXD) is one of the three instruments onboard Japanese X-ray astronomy satellite Astro-E2 scheduled for launch in 2005. This mission is very unique in a point of having a lower detector background than any other past missions in the 10-600 keV range. In the HXD, the large and thick BGO crystal are used as active shields for reducing the particle and gamma-ray background to the main detector. These anticoincidence shields are called as "Anti counters", which have a large geometrical area similar to 800 cm(2) and an uncollimated field of view of similar to 2 pi. Furthemore, they also have a larger effective area, corresponding to 400 cm(2) at even 1 MeV due to their thick high-Z materials. This feature enables us to observe the high energy radiation of Gamma-ray bursts with a higher sensitivity than previous all-sky monitors. Hence, the Anti counters have been developed as all-sky monitors with a broadband coverage of 50-5000 keV. In this paper, we will describe overall design of the HXD Anti counters, then report on the results of the pre-flight calibration test on June 2004 using the flight model. By irradiating various radio isotopes with Anti counters, we confirmed that they have capability as all-sky monitors. It is striking that the low energy threshold has been archived about 30 keV in spite of large volume of BGO scintillators.
  IEEE, English, International conference proceedings
  ISSN：1082-3654, Web of Science ID：WOS:000232002100064
• Development of a Monte Carlo simulator for the astro-E2 hard X-ray detector (HXD-II)　　　　　　　　　　　　　　　
  Yukikatsu Terada; Shin Watanabe; Masanori Ohno; Masaya Suzuki; Takeshi Itoh; Isao Takahashi; Goro Sato; Mio Murashin; Yasunobu Uchiyama; Shin Kubo; Tadayuki Takahashi; Makoto Tashiro; Motohide Kokubun; Kazuo Makishima; Tsuneyoshi Kamae; Toshio Murakami; Masaharu Nomach; Yasushi Fukazawa; Kazutaka Yamaoka; Kazuhiro Nakazawa; Daisuke Yonetoku
  IEEE Nuclear Science Symposium Conference Record, Volume：1, First page：395, Last page：399, 2004
  The Hard X-ray Detector (HXD-II) is one of the scientific payloads on board the fifth Japanese cosmic X-ray satellite Astro-E2, scheduled for launch in 2005. The HXD-II is designed to cover a wide energy range of 10 - 600 keV with a high sensitivity of ∼ 10-5 cnt/s/cm2/keV, using 16 identical GSO and BGO phoswich counters combined with 2 mm-thick silicon PIN diodes. In order to investigate the in-orbit performance of HXD-II in cosmic radiation environment, a Monte Carlo simulator based on the Geant4 toolkit is currently developed. There are two main goals of this simulator, which is directly connected to the detector's performance. One is to derive energy response to photons within the acceptance energy range, with 5% accuracy, after several types of standard event-selection of the HXD-II. The other is to estimate detector background with 10% accuracy. In addition to the background caused directly by the primary and secondary cosmic-rays, of particular importance is the radio-activation background induced by MeV protons trapped in the South Atlantic Anomaly. The simulator is also used in the pre-launch verifications of the HXD-II hardware. This paper describes the design concept of the Monte Carlo simulator, and its verification through comparison with the actual data of pre-flight radio-isotope irradiation experiments, together with calculated outputs that can demonstrate the in-orbit performance of the HXD-II. © 2004 IEEE.
  International conference proceedings
  Scopus：https://www.scopus.com/inward/record.uri?partnerID=HzOxMe3b&scp=23844551274&origin=inward
  Scopus Citedby：https://www.scopus.com/inward/citedby.uri?partnerID=HzOxMe3b&scp=23844551274&origin=inward
  ISSN：1095-7863, SCOPUS ID：23844551274
• Properties of CdZnTe detectors in the Burst Alert Telescope (BAT) array　　　　　　　　　　　　　　　
  G Sato; T Takahashi; K Nakazawa; S Watanabe; M Tashiro; M Suzuki; Y Okada; H Takahashi; A Parsons; J Tueller; H Krimm; S Barthelmy; J Cummings; C Markwardt; D Hullinger; N Gehrels; E Fenimore; D Palmer; T Dean; D Willis
  HARD X-RAY AND GAMMA-RAY DETECTOR PHYSICS V, Volume：5198, First page：209, Last page：216, 2004, [Reviewed]
  The properties of 32k CdZnTe detectors have been studied in the pre-flight calibration of Burst Alert Telescope (BAT) on-board the Swift Gamma-ray Burst Explorer (scheduled for launch in January 2004). After corrections of the linearity and the gain, the energy resolution of summed spectrum is 7.0 keV (FWHM) at 122 keV. In order to construct response matrices for the BAT instrument, we extracted mobility-lifetime (mutau) products for electrons and holes in the CdZnTe. Based on a new method applied to Co-57 spectra taken at different bias voltages, mutau for electrons ranges from 5.0 x 10(-4) to 1.0 X 10(-2) cm(2)V(-1), while mutau for holes ranges from 1.0 x 10(-5) to 1.7 x 10(-4) cm(2)V(-1). We show that the distortion of the spectrum and the peak efficiency of the BAT instrument are well reproduced by the mutau database constructed in the calibration.
  SPIE-INT SOC OPTICAL ENGINEERING, English, International conference proceedings
  ISSN：0277-786X, Web of Science ID：WOS:000189409400026
• Swift burst alert telescope (BAT) instrument response　　　　　　　　　　　　　　　
  A Parsons; S Barthelmy; J Cummings; N Gehrels; D Hullinger; H Krimm; C Markwardt; J Tueller; E Fenimore; D Palmer; G Sato; T Takahashi; K Nakazawa; Y Okada; H Takahashi; M Suzuki; M Tashiro
  GAMMA-RAY BURSTS: 30 YEARS OF DISCOVERY, Volume：727, First page：671, Last page：674, 2004, [Reviewed]
  The Burst Alert Telescope (BAT), a large coded aperture instrument with a wide field-of-view (FOV), provides the gamma-ray burst triggers and locations for the Swift Gamma-Ray Burst Explorer. In addition to providing this imaging information, BAT will perform a 15 keV - 150 keV all-sky hard x-ray survey based on the serendipitous pointings resulting from the study of gamma-ray bursts, and will also monitor the sky for transient hard x-ray sources. For BAT to provide spectral and photometric information for the gamma-ray bursts, the transient sources and the all-sky survey, the BAT instrument response must be determined to an increasingly greater accuracy. This paper describes the spectral models and the ground calibration experiments used to determine the BAT response to an accuracy suitable for gamma-ray burst studies.
  AMER INST PHYSICS, English, International conference proceedings
  ISSN：0094-243X, Web of Science ID：WOS:000224719700142
• Swift/BAT calibration and the estimated BAT hard x-ray survey sensitivity　　　　　　　　　　　　　　　
  A Parsons; J Tueller; H Krimm; S Barthelmy; J Cummings; C Markwardt; D Hullinger; N Gehrels; E Fenimore; D Palmer; G Sato; K Nakazawa; T Takahashi; S Watanabe; Y Okada; H Takahashi; M Suzuki; M Tashiro
  X-RAY AND GAMMA-RAY INSTRUMENTATION FOR ASTRONOMY XIII, Volume：5165, First page：190, Last page：200, 2004, [Reviewed]
  In addition to providing the initial gamma-ray burst trigger and location, the Swift Burst Alert Telescope (BAT) will also perform an all-sky hard x-ray survey based on serendipitous pointings resulting from the study of gamma-ray bursts. BAT was designed with a very wide field-of-view (FOV) so that it can observe roughly 1/7 of the sky at any time. Since gamma-ray bursts are uniformly distributed over the sky, the final BAT survey coverage is expected to be nearly uniform. BAT's large effective area and long sky exposures will produce a 15 - 150 keV survey with up to 30 times better sensitivity than any previous hard x-ray survey (e.g. HEAO A4). Since the sensitivity of deep exposures in this energy range is systematics limited, the ultimate survey sensitivity depends on the relative sizes of the statistical and systematic errors in the data. Many careful calibration experiments were performed at NASA/Goddard Space Flight Center to better understand the BAT instrument's response to 15-150 keV gamma-rays incident from any direction within the FOV. Using radioactive sources of gamma-rays with known locations and energies, the Swift team can identify potential systematic errors in the telescope's performance and estimate the actual Swift hard x-ray survey sensitivity in flight. These calibration results will be discussed and a preliminary parameterization of the BAT instrument response will be presented. While the details of the individual BAT CZT detector response will be presented elsewhere in these proceedings, this talk will focus on the translation of the calibration experimental data into overall hard x-ray survey sensitivity.
  SPIE-INT SOC OPTICAL ENGINEERING, English, International conference proceedings
  ISSN：0277-786X, Web of Science ID：WOS:000189441700021
• Swift status　　　　　　　　　　　　　　　
  M Tashiro; T Takahashi
  PROGRESS OF THEORETICAL PHYSICS SUPPLEMENT, Number：155, First page：429, Last page：430, 2004, [Reviewed]
  The gamma-ray burst (GRB) observatory Swift is now on the final stage of the prelaunch calibration to be launched in 2004. Swift is designed to observe GRBs and their afterglows with the burst alert telescope (BAT) and two multiwavelength telescopes (XRT and UVOT). The BAT, a coded mask hard X-ray telescope equipped with newly designed CdZnTe detectors, covers 1/6 sky to detect and determine the GRB position oriboard. With its sensitivity, it is calculated for the BAT to be able to detect more than 200 GRBs during its nominal two year mission life. The spacecraft maneuvers within about a minute to aim XRT and UVOT afterglows with their fine space and spectral resolutions. Swift is one of the ideal observatory to improve our knowledge by its capability of the continuous and multiwavelength observation. This paper also describes possible collaborations with X-ray and gamma-ray observatories including the coming ASTRO-E2.
  PROGRESS THEORETICAL PHYSICS PUBLICATION OFFICE, English, Scientific journal
  ISSN：0375-9687, Web of Science ID：WOS:000225350800104
• Response of CdZnTe detectors on the Swift burst alert telescope　　　　　　　　　　　　　　　
  M Suzuki; M Tashiro
  PROGRESS OF THEORETICAL PHYSICS SUPPLEMENT, Number：155, First page：421, Last page：422, 2004, [Reviewed]
  Swift (Gehrels, 2000) is the Gamma Ray Bursts (GRBs) explorer, that is scheduled for launch in 2004. The Swift's major instrument Burst Alert Telescope (BAT) detector array sits Cadmium Zinc Telluride (CdZnTe, CZT) semiconductor devices under a coded mask. The array has 32,768 individual Cd0.9Zn0.1Te1.0 detectors (4x4 mm(2) large, 2mm thick) that have a total detector area of 5240 cm(2). CdZnTe materials are able to operate at room temperature for its large band gap, and also have a high average atomic number which makes them sensitive to hard X-rays (15similar to150 keV). We investigate energy response of the BAT detector for which to dedicate spectroscopy and imaging in observations of GRBs.
  PROGRESS THEORETICAL PHYSICS PUBLICATION OFFICE, English, Scientific journal
  ISSN：0375-9687, Web of Science ID：WOS:000225350800100
• Hard X-ray response of CdZnTe detectors in the swift burst alert telescope　　　　　　　　　　　　　　　
  M Suzuki; M Tashiro; G Sato; S Watanabe; T Takahashi; Y Okada; F Takahashi; A Parsons; S Barthelmy; J Cummings; N Gehrels; D Hullinger; HF Krimm; J Tueller
  2003 IEEE NUCLEAR SCIENCE SYMPOSIUM, CONFERENCE RECORD, VOLS 1-5, First page：3550, Last page：3554, 2004, [Reviewed]
  The Burst Alert Telescope (BAT) onboard the Swift Gamma-ray Burst Explorer (scheduled for launch in May of 2004) has a coded aperture mask and a detector array of 32,768 Cd0.9Zn0.1Te1.0 (4x4mm(2) large, 2mm thick) semiconductor devices. Due to small mobility and short lifetime of carriers, the electron-hole pairs generated by irradiation of gamma-rays cannot be completely collected. Since the shape of the measured spectra has the broad low-energy tail, it is very useful for us to estimate the obtained spectra to fit the model which considers the charge transport properties depended on the depth of the photon interaction (G.Sato, 2002) [1]. The energy calibration of the BAT array and coded mask experiments were carried out at NASA/Goddard Space Flight Center between December 2002 and March 2003. We applied the model fitting to the calibration spectra, to yield the mobility-lifetime products for each detector and these values differ by over 2 orders of magnitude among detectors. Also using the mobility-lifetime parameters, we can identified the detector energy response as a function of the temperature and illumination angle. But we figure out a difference between the model and the obtained data. To determine the difference between the model and the measured data, we conducted the detailed check experiment for a single CdZnTe, to show that the cause of the excess is due to the areal nonuniformity of the mobility-lifetime parameter.
  IEEE, English, International conference proceedings
  ISSN：1082-3654, Web of Science ID：WOS:000223398000789
• Design and performance of soft gamma-ray detector for NeXT mission　　　　　　　　　　　　　　　
  Tajima H; Kamae T; Madejski G; Mitani T; Nakazawa K; Tanaka T; Takahashi T; Watanabe S; Fukazawa Y; Ikagawa T; Kataoka J; Kokubun M; Makishima K; Terada Y; Nomachi M; Tashiro M
  2004 IEEE Nuclear Science Symposium Conference Record, Vols 1-7, First page：314, Last page：321, 2004, [Reviewed]
  ISSN：1082-3654, Web of Science ID：WOS:000232002100065
• Preflight calibration and performance of the Astro-E2/HXD-II anti counter as the all sky monitor
  Ohno M; Fukazawa Y; Yamaoka K; Kokubun M; Terada Y; Kotoku J; Hong S; Mori M; Makishima K; Murakami T; Nakazawa K; Takahashi T; Tashiro M
  IEEE Nuclear Science Symposium Conference Record, Volume：1, First page：405, Last page：409, 2004, [Reviewed]
  ORCID：34407105, SCOPUS ID：23844556555
• Hard X-ray response of CdZnTe detectors in the swift burst alert telescope　　　　　　　　　　　　　　　
  Masaya Suzuki; Makoto Tashiro; Goro Sato; Shin Watanabe; Tadayuki Takahashi; Yuu Okada; Hiromitsu Takahashi; Ann Parsons; Scott Barthelmy; Jay Cummings; Neil Gehrels; Derek Hullinger; Hans Krimm; Jack Tueller
  IEEE Nuclear Science Symposium Conference Record, Volume：5, First page：3550, Last page：3554, 2003
  The Burst Alert Telescope (BAT) onboard the Swift Gamma-ray Burst Explorer (scheduled for launch in May of 2004) has a coded aperture mask and a detector array of 32,768 Cd 0.9Zn 0.1Te 1.0 (4×4mm 2 large, 2mm thick) semiconductor devices. Due to small mobility and short lifetime of carriers, the electron-hole pairs generated by irradiation of gamma-rays cannot be completely collected. Since the shape of the measured spectra has the broad low-energy tail, it is very useful for us to estimate the obtained spectra to fit the model which considers the charge transport properties depended on the depth of the photon interaction (G.Sato, 2002). The energy calibration of the BAT array and coded mask experiments were carried out at NASA/Goddard Space Flight Center between December 2002 and March 2003. We applied the model fitting to the calibration spectra, to yield the mobility-lifetime products for each detector and these values differ by over 2 orders of magnitude among detectors. Also using the mobility-lifetime parameters, we can identified the detector energy response as a fucntion of the temperature and illumination angle. But we figure out a difference between the model and the obtained data. To determine the difference between the model and the measured data, we conducted the detailed check experiment for a single CdZnTe, to show that the cause of the excess is due to the areal nonuniformity of the mobility-lifetime parameter.
  International conference proceedings
  Scopus：https://www.scopus.com/inward/record.uri?partnerID=HzOxMe3b&scp=19944425918&origin=inward
  Scopus Citedby：https://www.scopus.com/inward/citedby.uri?partnerID=HzOxMe3b&scp=19944425918&origin=inward
  ISSN：1095-7863, SCOPUS ID：19944425918
• ASCA observations of the northern outer lobe edge of the radio galaxy Centaurus A　　　　　　　　　　　　　　　
  N Isobe; K Makishima; M Tashiro; H Kaneda
  PARTICLES AND FIELDS IN RADIO GALAXIES, Volume：250, First page：394, Last page：399, 2002, [Reviewed]
  ASCA observation of the northern outer lobe edge region of the radio galaxy Centaurus A, similar to 3.5degrees north of its nucleus, is reported. Excess hard X-ray emission is seen around RA 13(hz)26m00(s), Dec. -39degrees20'00" (J2000 coordinates), together with soft diffuse X-ray emission extending all over the field of view of the GIS (similar to 50 arcmin in diameter). The spectrum of the soft diffuse emission is well described by an optically thin thermal plasma model with temperature kT similar to 0.6 keV modified by Galactic absorption. This emission is thought to arise from the thermal plasma associated with the outer lobe of Centaurus A and which has a thermal pressure of similar to 5 x 10(-13) dyn cm(-2). The excess hard emission is likely to be diffuse, and its spectrum is well described with a power law model of photon index similar to 1.7 or a thermal bremsstrahlung model of temperature kT greater than or similar to 11 keV. The nature of the hard emission is still unclear.
  ASTRONOMICAL SOC PACIFIC, English, International conference proceedings
  Web of Science ID：WOS:000178405600063
• Study of energy response of Gd2SiO5 : Ce3+scintillator for the ASTRO-E hard X-ray detector　　　　　　　　　　　　　　　
  Uchiyama, Y; Kouda, M; Tanihata, C; Isobe, N; Takahashi, T; Murakami, T; Tashiro, M; Makishima, K; Fukazawa, Y; Kamae, T
  IEEE TRANSACTIONS ON NUCLEAR SCIENCE, Volume：48, Number：3, First page：379, Last page：384, Jun. 2001, [Reviewed]
  The energy-dependent response of the crystalline oxide scintillator Gd2SiO5:Ce3+ (GSO:Ce) is studied in the energy range from 14 to 662 keV as a part of the preflight calibration of the hard X-ray detector (HXD) onboard the ASTRO-E satellite. In the relation between photon energy deposited and light yields, there exists nonproportionality and discontinuity around the energy of the gadolinium K-edge (50.2 keV). In 16 GSO scintillator units of the HXD flight model, the same characteristics of the energy response are confirmed. To evaluate the response across the K-edge quantitatively, we measure the electron response" by means of the Compton coincidence technique. By using the electron response of the GSO crystal, we calculate the light yield nonproportionality as a function of deposited photon energy. We find that a photopeak line profile of the 59.5-keV emission of Am-241 is well modeled by a composite Gaussian. This will be discussed in terms of the light yield nonproportionality."
  IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC, Scientific journal
  DOI：https://doi.org/10.1109/23.940084
  DOI ID：10.1109/23.940084, ISSN：0018-9499
• ASCA measurements of spatial distributions of magnetic field and electrons in the radio lobes of PKSB2356-601　　　　　　　　　　　　　　　
  M Tashiro; N Isobe; K Makishima; N Iyomoto; H Kaneda
  NEW CENTURY OF X-RAY ASTRONOMY, Volume：251, First page：416, Last page：417, 2001, [Reviewed]
  ASCA results are presented of extended X-rays from radio lobes of PKS B2356-601 and surrounding the cluster of galaxies Abell 4067. Obtained X-ray spectrum from the lobes allows two possibilities as its origin, those are a thin thermal plasma emission associated with one of lobes or an inverse-Compton (IC) emission by the relativistic electrons in the lobe. The paper presents a discussion on the origin and pressures of the lobe electrons and the surrounding intra-cluster medium.
  ASTRONOMICAL SOC PACIFIC, English, International conference proceedings
  Web of Science ID：WOS:000176731500135
• The HXD-II on Astro-E2: Another challenge to the hard X-ray sky　　　　　　　　　　　　　　　
  K Makishima; Y Fukazawa; T Kamae; M Kokubun; T Murakami; K Nakazawa; T Takahashi; M Tashiro; K Yamaoka
  NEW CENTURY OF X-RAY ASTRONOMY, Volume：251, First page：564, Last page：565, 2001, [Reviewed]
  A brief description is made of the HXD-II instrument, which is to be onboard the Astro-E2 mission to substitute the HXD (Hard X-ray Detector) instrument onboard the lost Astro-E.
  ASTRONOMICAL SOC PACIFIC, English, International conference proceedings
  Web of Science ID：WOS:000176731500207
• Relations between core luminosities and physical parameters of the lobes of radio galaxies　　　　　　　　　　　　　　　
  N Isobe; K Makishima; M Tashiro; H Kaneda; N Iyomoto
  NEW CENTURY OF X-RAY ASTRONOMY, Volume：251, First page：364, Last page：365, 2001, [Reviewed]
  The energy densities of electrons and magnetic fields, u(e) and u(m) respectively, are calculated for lobes of four radio galaxies from which the inverse Compton X-rays are detected. A tendency of u(e) > u(m) is found. Relations are examined between the core luminosity of radio galaxies and u(e) or u(m) in the lobes. We found that the ratio of u(e) to u(m) increases when the core becomes more active.
  ASTRONOMICAL SOC PACIFIC, English, International conference proceedings
  Web of Science ID：WOS:000176731500109
• Swift Burst Alert Telescope hard x-ray monitor and survey　　　　　　　　　　　　　　　
  HA Krimm; LM Barbier; SD Barthelmy; AJ Dean; A Eftekharzadeh; EE Fenimore; N Gehrels; DD Hullinger; H Ozawa; DM Palmer; AM Parsons; T Takahasi; M Tashiro; J Tueller; G Weidenspointner
  GAMMA 2001, Volume：587, First page：796, Last page：800, 2001, [Reviewed]
  The Burst Alert Telescope (BAT) on the Swift gamma-ray burst mission will perform the first new all sky hard x-ray survey since 1977. BAT is a coded aperture instrument with 17 arcminute pixels and a 2 ster partially coded field of view. The imaging area has 32768 CdZnTe detectors, each 4X4X2 mm, with a total area of 5243 cm(2). Swift will perform pointings covering >64% of the sky each day and achieve an integrated sensitivity in three years of 0.6 milliCrabs for sources well off the Galactic plane. This survey is expected to identify hundreds of new highly obscured AGN.
  AMER INST PHYSICS, English, International conference proceedings
  ISSN：0094-243X, Web of Science ID：WOS:000173389400140
• Nearly-final in-orbit calibration of the GIS onboard ASCA　　　　　　　　　　　　　　　
  M Tashiro; Y Ezoe; K Ebisawa; Y Fukazawa; T Furusho; E Idesawa; M Ishida; Y Ishisaki; H Kubo; A Kubota; K Makishima; T Ohashi; NY Yamasaki; T Yaqoob
  NEW CENTURY OF X-RAY ASTRONOMY, Volume：251, First page：592, Last page：593, 2001, [Reviewed]
  The nearly final in-orbit calibration of the GIS, installed on the focal plane of the X-ray astronomy satellite ASCA, are summarized. With the successive in-orbit calibration with celestial sources and comparison with the results from the SIS, the GIS team and ASCA-GOF performed fine recalibration resulting released four and a newly presented final versions energy response matrices in collaboration with the XRT, SIS and ASCA operation teams.
  ASTRONOMICAL SOC PACIFIC, English, International conference proceedings
  Web of Science ID：WOS:000176731500221
• Spectral evolution of PKS 2155-304 during the ASCA long-look campaign　　　　　　　　　　　　　　　
  M Kouda; C Tanihata; T Takahashi; M Tashiro; J Kataoka
  NEW CENTURY OF X-RAY ASTRONOMY, Volume：251, First page：376, Last page：377, 2001, [Reviewed]
  We collected all light curves of the TeV blazar PKS 2155-304, spanning over 12 years, obtained by both Ginga and ASCA. Taking the advantage that Ginga covers a higher energy range compared to ASCA, we confirmed the amplitude of the variations being larger at higher energies, which is consistent with the synchrotron picture of the X-ray jet. We also report on the recent ASCA continuous 10-day observation of this source. In spite of its low flux compared to previous observations, we detected significant daily variations, and found that there was actually no particular quiescent period throughout our observation.
  ASTRONOMICAL SOC PACIFIC, English, International conference proceedings
  Web of Science ID：WOS:000176731500115
• Achievements of the ASTRO-E hard X-ray detector development
  Tashiro M; Makishima K; Kamae T; Murakami T; Takahashi T; Fukazawa Y; Kokubun M; Nakazawa K; Nomachi M; Yoshida A; Ezoe Y; Isobe N; Iyomoto N; Kataoka J; Kotoku J; Kouda M; Kubo S; Kubota A; Matsumoto Y; Mizuno T; Okada Y; Ota N; Ozawa H; Sato G; Sugiho M; Sugizaki M; Takahashi I; Takahashi H; Tamura T; Tanihata C; Terada Y; Uchiyama Y; Watanabe S; Yamaoka K; Yonetoku D
  IEEE Nuclear Science Symposium and Medical Imaging Conference, Volume：1, First page：483, Last page：486, 2001, [Reviewed]
  The ASTRO-E Hard X-ray Detector utilized GSO/BGO well-type phoswich counters in compound-eye configuration [1], to achieve an extremely low background level of a few ×10-5 counts s-1cm-2keV-1. The GSO scintillators installed in the BGO active shield wells observes 30-600 keV photons, while silicon PIN diodes of 2 mm thick placed in front of each GSO crystal covers 10 - 60 keV photons with energy resolution of ∼3.5 keV FWHM. The design goals both of low background and high energy resolution in the hard X-ray bands were confirmed to be achieved through the preflight calibration experiments.
  International conference proceedings
  Scopus Citedby：https://www.scopus.com/inward/citedby.uri?partnerID=HzOxMe3b&scp=0035553511&origin=inward
  ORCID：34407088, SCOPUS ID：0035553511
• Spatially dependent response of thick and large area PIN diode developed for ASTRO-E hard x-ray detector　　　　　　　　　　　　　　　
  M. Sugiho; T. Kamae; K. Makishima; T. Takahashi; T. Murakami; M. Tashiro; Y. Fukazawa; M. Kaneda; T. Tamura; N. Iyomoto; M. Sugizaki; H. Ozawa; A. Kubota; K. Nakazawa; K. Yamaoka; M. Kokubun; N. Ota; C. Tanihata; N. Isobe; S. Kubo; Y. Terada; Y. Matsumoto; Y. Uchiyama; D. Yonetoku; I. Takahashi; J. Kotoku; S. Watanabe; Y. Ezoe
  IEEE Nuclear Science Symposium and Medical Imaging Conference, Volume：1, 2000
  The ASTRO-E Hard X-ray Detector utilizes GSO/BGO well-type phoswich counters in compound-eye configuration, to achieve an extremely low background level of about a few times 10-5 counts s-1 cm-2 keV-1. The GSO scintillators placed at the bottom of the BGO well observe photons in the energy range 30-600 keV. To cover the lower energy range of 10-60 keV, silicon PIN diodes of 2 mm in thickness and 21.5 × 21.5mm2 in size were newly developed, and placed in front of the GSO scintillators. The PIN diode exhibits complex spectral responses, including subpeak and low energy tail components. To examine the origin of these components, we measured spatially-resolved response of the PIN diode, and confirmed that the subpeak and the low energy tail are related to the electrode structures and electric fields in the PIN diode, respectively.
  International conference proceedings
  Scopus：https://www.scopus.com/inward/record.uri?partnerID=HzOxMe3b&scp=0034593751&origin=inward
  Scopus Citedby：https://www.scopus.com/inward/citedby.uri?partnerID=HzOxMe3b&scp=0034593751&origin=inward
  SCOPUS ID：0034593751
• ASCA observation of ultra-luminous X-ray sources and interpretation of their nature　　　　　　　　　　　　　　　
  T Mizuno; T Ohnishi; A Kubota; K Makishima; M Tashiro
  ASTRONOMISCHE NACHRICHTEN, Volume：320, Number：4-5, First page：356, Last page：356, 1999, [Reviewed]
  WILEY-V C H VERLAG GMBH, English, Scientific journal
  ISSN：0004-6337, Web of Science ID：WOS:000084277700118
• ASCA measurements of nonthermal pressures in the radio lobes　　　　　　　　　　　　　　　
  M Tashiro; N Iyomoto; H Kaneda; K Makishima; N Isobe
  ASTRONOMISCHE NACHRICHTEN, Volume：320, Number：4-5, First page：217, Last page：218, 1999, [Reviewed]
  A summary is presented of ASCA (Tanaka ct al. 1994) results on inverse-Comptonized X-rays from lobes of radio galaxies, which are emitted when relativistic electrons constructing synchrotron radio lobes boost up the cosmic microwave background photons to the X-ray and gamma-ray energy. By comparing the two radiation fluxes, we derived the energy distribution between magnetic fields and the relativistic electrons, assuming the same relativistic electrons in the lobes produce the emissions. This method is essentially free from the energy equipartition assumption. A study on spatial distributions of the field and particle energy densities is also presented. Based on the results presented in this paper, we suggest particle domination in the lobes and at the formation of the lobe.
  WILEY-V C H VERLAG GMBH, English, Scientific journal
  ISSN：0004-6337, Web of Science ID：WOS:000084277700019
• The digital data processing system of the ASTRO-E hard X-ray detector　　　　　　　　　　　　　　　
  Y Terada; M Tashiro; T Takahashi; Y Fukazawa; G Kawaguchi; K Matsuzaki; Odagi, I; Y Tanaka; K Makishima; T Kamae
  ASTRONOMISCHE NACHRICHTEN, Volume：320, Number：4-5, First page：377, Last page：377, 1999, [Reviewed]
  WILEY-V C H VERLAG GMBH, English, Scientific journal
  ISSN：0004-6337, Web of Science ID：WOS:000084277700139
• ASCA observation of the BL Lac object PKS 1413+135 embedded in a spiral galaxy　　　　　　　　　　　　　　　
  M Sugiho; M Tashiro; ES Perlman; K Makishima; JT Stocke; QD Wang; G Madejski
  ASTRONOMISCHE NACHRICHTEN, Volume：320, Number：4-5, First page：316, Last page：316, 1999, [Reviewed]
  WILEY-V C H VERLAG GMBH, English, Scientific journal
  ISSN：0004-6337, Web of Science ID：WOS:000084277700078
• ASCA observations of blazars and multiband analysis　　　　　　　　　　　　　　　
  H Kubo; T Takahashi; G Madejski; F Makino; M Tashiro
  ASTROPHYSICAL LETTERS & COMMUNICATIONS, Volume：39, Number：1-6, First page：549, Last page：552, 1999, [Reviewed]
  We present multiband data for 18 blazars observed with ASCA, half of which were also observed contemporaneously with EGRET as parts of multi-wavelength campaigns. The ASCA X-ray spectra of High-energy peaked BL Lacs (HBLs) are soft, and they form the highest energy tail of the low energy (synchrotron) component. The X-ray spectra of the quasar-hosted blazars (QHBs) are hard and consistent with the lowest energy end of the high energy (HE, Compton) component. For Low-energy peaked BL Lacs (LBLs), the X-ray spectra are intermediate. We find that the radiation process responsible for the HE peak for HBLs can be explained solely by Synchrotron-Self-Compton (SSC) emission. For many QHBs, on the other hand, the gamma-rays cannot be solely due to the SSC mechanism. We consider an alternative scenario for QHBs where the SSC component dominates in the X-ray band, but it is below the observed gamma-ray spectrum. We infer the magnetic field to be 0.1 - 1 Gauss, and Lorentz factors of electrons radiating at the peak of the vF(v) spectrum of 10(3) for QHBs. This is much lower than 10(5) for HBLs. This difference is most likely due to the large photon density expected in QHBs.
  GORDON BREACH SCI PUBL LTD, English, Scientific journal
  ISSN：0888-6512, Web of Science ID：WOS:000089508200018
• Thick and large area PIN diodes for hard X-ray astronomy
  Ota N; Murakami T; Sugizaki M; Kaneda M; Tamura T; Ozawa H; Kamae T; Makishima K; Takahashi T; Tashiro M; Fukazawa Y; Kataoka J; Yamaoka K; Kubo S; Tanihata C; Uchiyama Y; Matsuzaki K; Iyomoto N; Kokubun M; Nakazawa T; Kubota A; Mizuno T; Matsumoto Y; Isobe N; Terada Y; Sugiho M; Onishi T; Kubo H; Ikeda H; Nomachi M; Ohsugi T; Muramatsu M; Akahori H
  Nuclear Instruments and Methods in Physics Research, Section A: Accelerators, Spectrometers, Detectors and Associated Equipment, Volume：436, Number：1-2, First page：291, Last page：296, 1999, [Reviewed]
  Thick and large area PIN diodes for the hard X-ray astronomy in the 10-60 keV range are developed. To cover this energy range in a room temperature and in a low background environment, Si PIN junction diodes of 2 mm in thickness with 2.5 cm2 in effective area were developed, and will be used in the bottom of the Phoswich Hard X-ray Detector (HXD), on-board the ASTRO-E satellite. Problems related to a high purity Si and a thick depletion layer during our development and performance of the PIN diodes are presented in detail.
  Scientific journal
  DOI：https://doi.org/10.1016/S0168-9002(99)00636-1
  Scopus Citedby：https://www.scopus.com/inward/citedby.uri?partnerID=HzOxMe3b&scp=0343496826&origin=inward
  DOI ID：10.1016/S0168-9002(99)00636-1, ISSN：0168-9002, ORCID：34407221, SCOPUS ID：0343496826
• Fabrication of the ASTRO-E Hard X-ray detector
  Nakazawa K; Kamae T; Makishima K; Takahashi T; Murakami T; Tashiro M; Fukazawa Y; Tamura T; Iyomoto N; Ebisawa K; Ezoe Y; Hamaya M; Horii M; Isobe N; Kokubun M
  Proceedings of SPIE - The International Society for Optical Engineering, Volume：3765, First page：148, Last page：159, 1999, [Reviewed]
  ORCID：34407116, SCOPUS ID：0033354596
• Activation of the ASTRO-E hard X-ray detector in low Earth orbit
  Kokubun M; Fukazawa Y; Idesawa E; Kataoka J; Kamae T; Matsuzaki K; Mizuno T; Saito Y; Takahashi T; Takizawa K; Tashiro M; Tamura T; Yoshida A
  IEEE Nuclear Science Symposium and Medical Imaging Conference, Volume：1, First page：227, Last page：232, 1999, [Reviewed]
  ASTRO-E Hard X-ray Detector (HXD) is characterized by well-type phoswich counters in a compound-eye configuration which reduce the X-ray and non X-ray background to lower level than any other past hard X-ray missions. When operating in Low Earth Orbit, the expected background of the HXD is an order of 10-5[counts/s/keV/cm2], mainly caused from the radioactivity induced within the detector materials by nuclear interactions with geomagnetically trapped protons. Results are presented from measurements of induced radioactivity in two phoswich scintillators, GSO and BGO, irradiated by mono-energetic protons at an accelerator facility. Radiation transport computer codes are used to build the detector response functions against emissions from decays of spallation products. Based on the comparison of experimental and simulation results, the activation background level of HXD in the orbit is estimated.
  Scientific journal
  Scopus Citedby：https://www.scopus.com/inward/citedby.uri?partnerID=HzOxMe3b&scp=0032597258&origin=inward
  ORCID：34407104, SCOPUS ID：0032597258
• High energy emission from blazars - ASCA observation of blazars and multiband analysis　　　　　　　　　　　　　　　
  T Takahashi; H Kubo; G Madejski; M Tashiro; F Makino
  OBSERVATIONAL PLASMA ASTROPHYSICS: FIVE YEARS OF YOHKOH AND BEYOND, Volume：229, First page：61, Last page：70, 1998, [Reviewed]
  SPRINGER, English, International conference proceedings
  Web of Science ID：WOS:000073874900010
• Evidence for a dramatic activity decline in the nucleus of the radio galaxy Fornax A　　　　　　　　　　　　　　　
  N Iyomoto; K Makishima; M Tashiro; K Matsushita; Y Fukazawa; H Kaneda; S Osone
  HOT UNIVERSE, Number：188, First page：446, Last page：446, 1998, [Reviewed]
  KLUWER ACADEMIC PUBL, English, Scientific journal
  ISSN：0074-1809, Web of Science ID：WOS:000077472500166
• ASCA x-ray observation of the lobe dominant radio galaxy NGC 612　　　　　　　　　　　　　　　
  M Tashiro; H Kaneda; K Makishima
  HOT UNIVERSE, Number：188, First page：289, Last page：290, 1998, [Reviewed]
  KLUWER ACADEMIC PUBL, English, Scientific journal
  ISSN：0074-1809, Web of Science ID：WOS:000077472500089
• Electronic system for the Astro-E Hard X-ray Detector　　　　　　　　　　　　　　　
  T. Takahashi; M. Nomachi; Y. Fukazawa; M. Tashiro; H. Ezawa; M. Hamaya; M. Horii; N. Isobe; N. Iyomoto; J. Kataoka; T. Kamae; G. Kawaguchi; H. Kubo; S. Kubo; A. Kubota
  Proceedings of SPIE - The International Society for Optical Engineering, Volume：3445, First page：155, Last page：168, 1998, [Reviewed]
  English
• Verification of the Astro-E Hard X-ray Detector based on newly developed Ground Support Equipment　　　　　　　　　　　　　　　
  J. Kataoka; M. Nomachi; T. Takahashi; G. Kawaguchi; Y. Terada; T. Murakami; C. Tanihata; Y. Uchiyama; K. Yamaoka; Y. Fukazawa; T. Kamae; K. Makishima; M. Tashiro; H. Kubo
  Proceedings of SPIE - The International Society for Optical Engineering, Volume：3445, First page：143, Last page：154, 1998, [Reviewed]
  We report the first results of the ground test of the Hard X-ray Detector (HXD) on board the Astro-E mission, by means of the newly developed Ground Support Equipment (GSE). Astro-E will be launched in 2000 by a Japanese M-V rocket. In order to verify the detector system during the limited time before launch, fast and versatile GSE is necessary. For this, we have developed a flexible test system based on nine VME I/O boards for a SUN workstation. These boards carry reconfigurable Field Programmable Gate Arrays (FPGAs) with 50,000 gates, together with 1 Mbyte SRAM devices tightly coupled to each FPGA device. As an application of using this GSE, we have tested the performance of a phoswich unit of the Flight Model of the HXD. In this paper, we present a schematic view of the GSE highlighting the functional design, and the results of our ground test of the HXD-sensor under the high count rate environment (approximately 10 kHz/unit) expected in orbit.
  English, International conference proceedings
  Scopus：https://www.scopus.com/inward/record.uri?partnerID=HzOxMe3b&scp=0032299383&origin=inward
  Scopus Citedby：https://www.scopus.com/inward/citedby.uri?partnerID=HzOxMe3b&scp=0032299383&origin=inward
  ISSN：0277-786X, SCOPUS ID：0032299383
• ASCA observations of blazars and multiband analysis　　　　　　　　　　　　　　　
  T Takahashi; H Kubo; G Madejski; M Tashiro; F Makino
  PROCEEDINGS OF THE FOURTH COMPTON SYMPOSIUM, PTS 1 AND 2, Number：410, First page：1467, Last page：1471, 1997, [Reviewed]
  We present results of multiband analysis for 18 blazars observed with the X-ray satellite ASCA, half of which were also observed contemporaneously with EGRET instrument onboard Compton Gamma-ray Observatory (CGRO). Our multi-band analysis suggests that the magnetic field is 0.1 similar to 1 gauss. With these values of B, we estimate gamma(b) is 10(3) similar to 10(4) for quasar-hosted blazars (QHBs), and 10(5) for X-ray selected BL Lac objects (HBLs).
  AMER INST PHYSICS, English, International conference proceedings
  ISSN：0094-243X, Web of Science ID：WOS:000071400800217
• X-ray observations of low luminosity active galactic nuclei in elliptical galaxies　　　　　　　　　　　　　　　
  N Iyomoto; K Makishima; K Matsushita; Y Fukazawa; M Tashiro; T Ohashi
  SECOND STROMLO SYMPOSIUM: THE NATURE OF ELLIPTICAL GALAXIES, Volume：116, First page：409, Last page：410, 1997, [Reviewed]
  ASTRONOMICAL SOC PACIFIC, English, International conference proceedings
  Web of Science ID：WOS:000073252500084
• Development of the large area silicon PIN diode with 2 mm-thick depletion layer for hard X-ray detector (HXD) on-board ASTRO-E
  Sugizaki M; Kubo S; Murakami T; Ota N; Ozawa H; Takahashi T; Kaneda H; Iyomoto N; Kamae T; Kokubun M; Kubota A; Makishima K; Tamura T; Tashiro M; Koyama K; Tsunemi H
  Proceedings of SPIE - The International Society for Optical Engineering, Volume：3115, First page：244, Last page：253, 1997, [Reviewed]
  DOI：https://doi.org/10.1117/12.277691
  DOI ID：10.1117/12.277691, ORCID：34407241, SCOPUS ID：0001331405
• Gamma-ray burst monitoring with the hard X-ray detector onboard the ASTRO-E mission　　　　　　　　　　　　　　　
  A Yoshida; H Ezawa; Y Fukazawa; M Hirayama; E Idesawa; H Ikeda; Y Ishisaki; N Iyomoto; T Kamae; J Kataoka; H Kaneda; H Kubo; K Makishima; K Matsushita; K Matsuzaki; T Mizuno; T Murakami; K Nagata; S Nakamae; M Nomachi; H Obayashi; T Otsuka; H Ozawa; Y Saito; M Sugizaki; T Takahashi; T Tamura; M Tashiro; N Tsuchida; K Tsukada
  GAMMA-RAY BURSTS - 3RD HUNTSVILLE SYMPOSIUM, PTS 1 AND 2, Number：384, First page：870, Last page：874, 1996, [Reviewed]
  ASTRO-E is the fifth Japanese X-ray astronomy satellite scheduled to be launched in year 2000. The satellite will carry three scientific instruments, one of which is the Hard X-ray Detector (HXD). HXD will cover the 10-600 keV band with low background of several x 10(-6)c/s/cm(2)/keV. This will be achieved by the well-type phoswich counter technique together with large active shield counters of EGO (about 1200 cm(2)/side), which are also capable to detect GRBs in the 100-2000 keV band. About 100 GRBs are expected to be detected per year with HXD.
  AIP PRESS, English, International conference proceedings
  ISSN：0094-243X, Web of Science ID：WOS:A1996BH28Y00169
• Development of the hard X-ray detector for the ASTRO-E mission　　　　　　　　　　　　　　　
  H KANEDA; H EZAWA; M HIRAYAMA; T KAMAE; H KUBO; K MATSUZAKI; K MAKISHIMA; T OHTSUKA; Y SAITO; Y SEKIMOTO; T TAKAHASHI; T TAMURA; M TASHIRO; N TSUCHIDA
  EUV, X-RAY, AND GAMMA-RAY INSTRUMENTATION FOR ASTRONOMY VI, Volume：2518, First page：85, Last page：95, 1995, [Reviewed]
  SPIE - INT SOC OPTICAL ENGINEERING, English, International conference proceedings
  Web of Science ID：WOS:A1995BE21T00007
• In-orbit performance of the GIS instrument on-board ASCA (ASTRO-D)　　　　　　　　　　　　　　　
  TASHIRO M; MAKISHIMA K; EZAWA H; FUKAWA Y; IDESAWA E; ISHISAKI Y; IYOMOTO N; KAMAE T; KANEDA H; MATSUSHITA K; MATSUZAKI K; SAITO Y; SEKIMOTO Y; TAMURA T; HIRAYAMA M; ISHIDA M; KUBO H; OKADA K; TAKAHASHI T; UEDA Y; KIKUCHI K; OHASHI T; YAMASAKI NY; KOHMURA Y; IKEBE Y; MIHARA T; TSURU T; EBISAWA K; GUNJI S
  EUV, X-RAY, AND GAMMA-RAY INSTRUMENTATION FOR ASTRONOMY VI, Volume：2518, First page：2, Last page：12, 1995, [Reviewed]
  The fourth Japanese x-ray astronomy satellite, ASCA, carries two imaging gas scintillation proportional counters (GIS) on its focal plane. Extensive ground calibration has established its position resolution to be 0.5 mm and FWHM energy resolution to be 8.0% both at 6 keV. When combined with the x-ray telescope, a sensitivity range becomes 0.7 - 10 keV. These properties have been confirmed through in-orbit calibrations. The in-orbit background of the GIS has been confirmed to be as low as (5 - 7) × 10 -4 c s -1cm -2keV -1 over the 1 - 10 keV range. The long-term detector gain is stable within a few % for two years. Gain dependence on the position and temperature has been calibrated down to 1%. The overall energy response is calibrated very accurately. Thus the GIS is working as an all-round cosmic x-ray detector.
  International conference proceedings
  DOI：https://doi.org/10.1117/12.218370
  Scopus：https://www.scopus.com/inward/record.uri?partnerID=HzOxMe3b&scp=0029537973&origin=inward
  Scopus Citedby：https://www.scopus.com/inward/citedby.uri?partnerID=HzOxMe3b&scp=0029537973&origin=inward
  DOI ID：10.1117/12.218370, ISSN：0277-786X, SCOPUS ID：0029537973, Web of Science ID：WOS:A1995BE21T00001
• CALIBRATIONS OF IMAGING GAS SCINTILLATION PROPORTIONAL-COUNTERS ON ASTRO-D　　　　　　　　　　　　　　　
  Y KOHMURA; Y FUKAZAWA; Y IKEBE; Y ISHISAKI; S KAMIJO; H KANEDA; K MAKISHIMA; K MATSUSHITA; K NAKAGAWA; M TASHIRO; T OHASHI; H INOUE; M ISHIDA; F MAKINO; T MURAKAMI; Y OGAWARA; Y TANAKA; Y UEDA; K EBISAWA; T MIHARA; T TAKESHIMA; T TSURU; K HIYOSHI; M HORII; R SHOUMURA; K TAGUCHI
  EUV, X-RAY, AND GAMMA-RAY INSTRUMENTATION FOR ASTRONOMY IV, Volume：2006, First page：78, Last page：89, 1993, [Reviewed]
  SPIE - INT SOC OPTICAL ENGINEERING, English, International conference proceedings
  Web of Science ID：WOS:A1993BZ57B00009
• IMAGING GAS SCINTILLATION PROPORTIONAL-COUNTERS FOR ASTRO-D　　　　　　　　　　　　　　　
  T OHASHI; K MAKISHIMA; M ISHIDA; T TSURU; M TASHIRO; T MIHARA; Y KOHMURA; H INOUE
  EUV, X-RAY, AND GAMMA-RAY INSTRUMENTATION FOR ASTRONOMY II, Volume：1549, First page：9, Last page：19, 1991, [Reviewed]
  SPIE - INT SOC OPTICAL ENGINEERING, English, International conference proceedings
  Web of Science ID：WOS:A1991BU57P00002

• X線分光撮像衛星XRISMの科学運用の現状(2)　　　　　　　　　　　　　　　
  吉田鉄生; 林克洋; 金丸善朗; 小川翔司; 福島光太郎; 寺田幸功; 田代信; 高橋弘充; 水野恒史; 深沢泰司; 阪本菜月; 信川正順; 宇野伸一郎; 中澤知洋; 大宮悠希; 大熊佳吾; 内山秀樹; 久保田あや; 勝田哲; 塩入匠; 本上侑吾; 寺島雄一; 志達めぐみ; 新居田祐基; 高木利紘; 山内茂雄; 太田直美; 白木天音; 鈴木那梨; 北口貴雄; 山田智史; 坪井陽子; 米山友景; 根本登; 内田悠介; 江口智士; 谷本敦; 善本真梨那; 内田和海; 海老沢研; 渡辺伸; 飯塚亮; HOLLAND Matt; YAQOOB Tahir; BALUTA Chris; LOEWENSTEIN Michael; LOEWENSTEIN Michael; MILLER Eric
  Volume：2024, 2024
  ISSN：1347-0639, J-Global ID：202402236287409494
• Current Status of the XRISM Science Operations: II　　　　　　　　　　　　　　　
  林克洋; 田代信; 田代信; 寺田幸功; 寺田幸功; 高橋弘充; 信川正順; 水野恒史; 宇野伸一郎; 中澤知洋; 内山秀樹; 久保田あや; 寺島雄一; 深澤泰司; 山内茂雄; 太田直美; 北口貴雄; 勝田哲; 坪井陽子; 志達めぐみ; 海老沢研; 内田悠介; 江口智士; 谷本敦; 米山友景; 山田智史; 内田和海; 吉田鉄生; 金丸善朗; 小川翔司; 福島光太郎; 渡辺伸; 飯塚亮; HOLLAND Matt; LOEWENSTEIN Michael; LOEWENSTEIN Michael; MILLER Eric; YAQOOB Tahir; BALUTA Chris; 白木天音; 新居田祐基; 根本登; 大宮悠希; 鈴木那梨; 善本真梨那; 大熊佳吾; 本上侑吾; 高木利紘
  日本物理学会講演概要集(CD-ROM), Volume：79, Number：2, 2024
  ISSN：2189-079X, J-Global ID：202502277995798054
• X線分光撮像衛星XRISMの科学運用の現状　　　　　　　　　　　　　　　
  小川翔司; 寺田幸功; 田代信; 高橋弘充; 水野恒史; 深沢泰司; 阪本菜月; 信川正順; 宇野伸一郎; 中澤知洋; 大宮悠希; 大熊佳吾; 内山秀樹; 久保田あや; 勝田哲; 塩入匠; 寺島雄一; 志達めぐみ; 新居田祐基; 山内茂雄; 太田直美; 白木天音; 鈴木那梨; 北口貴雄; 山田智史; 坪井陽子; 米山友景; 根本登; 内田悠介; 江口智士; 谷本敦; 善本真梨那; 海老沢研; 渡辺伸; 飯塚亮; 林克洋; 内田和海; 金丸善朗; 星野晶夫; 吉田鉄生; HOLLAND Matt; YAQOOB Tahir; BALUTA Chris; LOEWENSTEIN Michael; LOEWENSTEIN Michael; MILLER Eric
  Volume：2024, 2024
  ISSN：1347-0639, J-Global ID：202402268559182117
• Current Status of the XRISM Science Operations　　　　　　　　　　　　　　　
  林克洋; 田代信; 田代信; 寺田幸功; 寺田幸功; 高橋弘充; 信川正順; 水野恒史; 宇野伸一郎; 中澤知洋; 内山秀樹; 久保田あや; 寺島雄一; 深澤泰司; 山内茂雄; 太田直美; 北口貴雄; 勝田哲; 坪井陽子; 志達めぐみ; 海老沢研; 内田悠介; 江口智士; 谷本敦; 米山友景; 山田智史; 内田和海; 吉田鉄生; 金丸善朗; 小川翔司; 星野晶夫; 渡辺伸; 飯塚亮; HOLLAND Matt; LOEWENSTEIN Michael; LOEWENSTEIN Michael; MILLER Eric; YAQOOB Tahir; BALUTA Chris; 塩入匠; 阪本菜月; 白木天音; 新居田祐基; 根本登; 大宮悠希; 鈴木那梨; 善本真梨那; 大熊佳吾
  日本物理学会講演概要集(CD-ROM), Volume：79, Number：1, 2024
  ISSN：2189-079X, J-Global ID：202402253520919847
• XRISM Timing System and in-orbit Verification　　　　　　　　　　　　　　　
  寺田幸功; 寺田幸功; 志達めぐみ; 塩入匠; 新居田祐基; 澤田真理; 小湊隆; 田代信; 田代信; 戸田謙一; 前島弘則; 夏苅権; 高橋弘充; 信川正順; 水野恒史; 宇野伸一郎; 中澤知洋; 内山秀樹; 久保田あや; 寺島雄一; 深沢泰司; 山内茂雄; 太田直美; 北口貴雄; 勝田哲; 坪井陽子; 海老沢研; 内田悠介; 江口智士; 林克洋; 谷本敦; 米山友景; 山田智史; 内田和海; 吉田鉄生; 金丸善朗; 小川翔司; 星野晶夫; 渡辺伸; 飯塚亮; HOLLAND M; LOEWENSTEIN M; LOEWENSTEIN M; MILLER E; YAQOOB T; BALUTA C
  日本物理学会講演概要集(CD-ROM), Volume：79, Number：1, 2024
  ISSN：2189-079X, J-Global ID：202402277873851601
• X線分光撮像衛星XRISMの科学運用に向けての模擬試験　　　　　　　　　　　　　　　
  林克洋; 田代信; 田代信; 寺田幸功; 寺田幸功; 高橋弘充; 信川正順; 水野恒史; 宇野伸一郎; 久保田あや; 中澤知洋; 渡辺伸; 飯塚亮; 佐藤理江; 米山友景; 吉田鉄生; BALUTA Chris; 海老沢研; 江口智士; 深澤泰司; 橋口葵; 勝田哲; 北口貴雄; 小高裕和; 大野雅功; 太田直美; 阪間美南; 阪本菜月; 志達めぐみ; 塩入匠; 丹波翼; 谷本敦; 寺島雄一; 坪井陽子; 内田和海; 内田悠介; 内山秀樹; 山田智史; 山内茂雄
  Volume：2023, 2023
  ISSN：1347-0639, J-Global ID：202302210598711687
• X線分光撮像衛星XRISMの観測データ処理ツールの開発状況　　　　　　　　　　　　　　　
  山田智史; 田代信; 田代信; 寺田幸功; 寺田幸功; 高橋弘充; 信川正順; 水野恒史; 宇野伸一郎; 久保田あや; 中澤知洋; 渡辺伸; 飯塚亮; 佐藤理江; 林克洋; 米山友景; 吉田鉄生; BALUTA Chris; 海老沢研; 江口智士; 深澤泰司; 橋口葵; 勝田哲; 北口貴雄; 小高裕和; 大野雅功; 太田直美; 阪間美南; 阪本菜月; 志達めぐみ; 塩入匠; 丹波翼; 谷本敦; 寺島雄一; 坪井陽子; 内田和海; 内田悠介; 内山秀樹; 山内茂雄
  Volume：2023, 2023
  ISSN：1347-0639, J-Global ID：202302249250042517
• X線分光撮像衛星XRISMの科学運用準備の現状(2)　　　　　　　　　　　　　　　
  米山友景; 田代信; 田代信; 寺田幸功; 寺田幸功; 高橋弘充; 信川正順; 水野恒史; 宇野伸一郎; 久保田あや; 中澤知洋; 渡辺伸; 飯塚亮; 佐藤理江; 林克洋; 吉田鉄生; BALUTA Chris; 海老沢研; 江口智士; 深澤泰司; 橋口葵; 勝田哲; 北口貴雄; 小高裕和; 大野雅功; 太田直美; 阪間美南; 阪本菜月; 志達めぐみ; 塩入匠; 丹波翼; 谷本敦; 寺島雄一; 坪井陽子; 内田和海; 内田悠介; 内山秀樹; 山田智史; 山内茂雄
  Volume：2023, 2023
  ISSN：1347-0639, J-Global ID：202302258897086050
• Status report of the XRISM science operation　　　　　　　　　　　　　　　
  内田悠介; 田代信; 田代信; 寺田幸功; 寺田幸功; 高橋弘充; 信川正順; 水野恒史; 宇野伸一郎; 久保田あや; 中澤知洋; 渡辺伸; 飯塚亮; 佐藤理江; 米山友景; 吉田鉄生; BALUTA Chris; 海老沢研; 江口智士; 深澤泰司; 橋口葵; 林克洋; 勝田哲; 北口貴雄; 小高裕和; 大野雅功; 太田直美; 阪間美南; 阪本菜月; 志達めぐみ; 塩入匠; 丹波翼; 谷本敦; 寺島雄一; 坪井陽子; 内田和海; 内山秀樹; 山田智史; 山内茂雄
  日本物理学会講演概要集(CD-ROM), Volume：78, Number：1, 2023
  ISSN：2189-079X, J-Global ID：202302211107124079
• X線分光撮像衛星XRISMの科学運用準備の現状(3)　　　　　　　　　　　　　　　
  林克洋; 田代信; 寺田幸功; 高橋弘充; 信川正順; 水野恒史; 宇野伸一郎; 久保田あや; 中澤知洋; 渡辺伸; 飯塚亮; 佐藤理江; 星野晶夫; 吉田鉄生; 小川翔司; 金丸善朗; BALUTA Chris; 海老沢研; 江口智士; 小高裕和; 勝田哲; 北口貴雄; 新居田祐基; 太田直美; 阪本菜月; 志達めぐみ; 塩入匠; 白木天音; 谷本敦; 寺島雄一; 坪井陽子; 内田和海; 内田悠介; 内山秀樹; 山田智史; 山内茂雄; 米山友景
  Volume：2023, 2023
  ISSN：1347-0639, J-Global ID：202302259844930637
• MAGIC報告66:HESS J1912+101領域のガンマ線放射　　　　　　　　　　　　　　　
  永吉勤; 永吉勤; GREEN David; FRUCK Christian; STRZYS Marcel; 井上進; 稲田知大; 岩村由樹; 大谷恵生; 岡知彦; 緒方智之; 神本匠; 梶原由貴; 櫛田淳子; 窪秀利; 久門拓; 小林志鳳; 齋藤隆之; 櫻井駿介; 高橋光成; 種田裕貴; 辻本晋平; 手嶋政廣; 手嶋政廣; 中森健之; 西嶋恭司; 野崎誠也; 野田浩司; HADASCH Daniela; 平子丈; 深見哲志; 古田智也; MAZIN Daniel; MAZIN Daniel; 増田周; 勝田哲; 佐藤浩介; 田代信; 寺田幸功
  Volume：74, Number：1, 2019
  ISSN：2189-079X, J-Global ID：201902219247405378
• X線衛星代替機XARMにおける科学運用計画
  寺田幸功; 田代信; 田代信; 海老沢研; 深沢泰司; 飯塚亮; 勝田哲; 北口貴雄; 久保田あや; 水野恒史; 中島真也; 中澤知洋; 信川正順; 大野雅功; 太田直美; 志達めぐみ; 菅原泰晴; 高橋弘充; 田村隆幸; 田中康之; 寺島雄一; 坪井陽子; 内山秀樹; 宇野伸一郎; 渡辺伸; 山内茂雄
  日本天文学会年会講演予稿集, Volume：2018, First page：228, 20 Feb. 2018
  Japanese
  ISSN：1347-0639, J-Global ID：201802220528606681
• 電波銀河Pictor Aの西ホットスポットの遠赤外線超過の検出　　　　　　　　　　　　　　　
  磯部直樹; 小山翔子; 紀基樹; 中川貴雄; 田代信; 田代信; 永井洋; PEARSON Chris
  Volume：2018, 2018
  ISSN：1347-0639, J-Global ID：201802284604343172
• Concept of the X-ray Astronomy Recovery Mission
  Makoto Tashiro; Makoto Tashiro; Hironori Maejima; Kenichi Toda; Richard Kelley; Lillian Reichenthal; James Lobell; Robert Petre; Matteo Guainazzi; Elisa Costantini; Mark Edison; Ryuichi Fujimoto; Martin Grim; Kiyoshi Hayashida; Jan Willem Den Herder; Yoshitaka Ishisaki; Stéphane Paltani; Kyoko Matsushita; Koji Mori; Gary Sneiderman; Yoh Takei; Yukikatsu Terada; Hiroshi Tomida; Hiroki Akamatsu; Lorella Angelini; Yoshitaka Arai; Hisamitsu Awaki; Lurli Babyk; Lurli Babyk; Aya Bamba; Peter Barfknecht; Kim Barnstable; Thomas Bialas; Branimir Blagojevic; Joseph Bonafede; Clifford Brambora; Laura Brenneman; Greg Brown; Kimberly Brown; Laura Burns; Edgar Canavan; Tim Carnahan; Meng Chiao; Brian Comber; Lia Corrales; Cor De Vries; Johannes Dercksen; Maria DIaz-Trigo; Tyrone DIllard; Michael DIpirro; Chris Done; Tadayasu Dotani; Ken Ebisawa; Megan Eckart; Teruaki Enoto; Yuichiro Ezoe; Carlo Ferrigno; Yutaka Fujita; Yasushi Fukazawa; Akihiro Furuzawa; Luigi Gallo; Steve Graham; Liyi Gu; Kohichi Hagino; Kenji Hamaguchi; Isamu Hatsukade; Dean Hawes; Takayuki Hayashi; Cailey Hegarty; Natalie Hell; Junko Hiraga; Edmund Hodges-Kluck; Matt Holland; Ann Hornschemeier; Akio Hoshino; Yuto Ichinohe; Ryo Iizuka; Kazunori Ishibashi; Manabu Ishida; Kumi Ishikawa; Kosei Ishimura; Bryan James; Timothy Kallman; Erin Kara; Satoru Katsuda; Steven Kenyon; Caroline Kilbourne; Mark Kimball; Takao Kitaguchi; Shunji Kitamoto; Shogo Kobayashi; Takayoshi Kohmura; Shu Koyama; Aya Kubota; Maurice Leutenegger; Maurice Leutenegger; Tom Lockard; Mike Loewenstein; Yoshitomo Maeda; Lynette Marbley
  Proceedings of SPIE - The International Society for Optical Engineering, Volume：10699, 01 Jan. 2018
  © 2018 SPIE. The ASTRO-H mission was designed and developed through an international collaboration of JAXA, NASA, ESA, and the CSA. It was successfully launched on February 17, 2016, and then named Hitomi. During the in-orbit verification phase, the on-board observational instruments functioned as expected. The intricate coolant and refrigeration systems for soft X-ray spectrometer (SXS, a quantum micro-calorimeter) and soft X-ray imager (SXI, an X-ray CCD) also functioned as expected. However, on March 26, 2016, operations were prematurely terminated by a series of abnormal events and mishaps triggered by the attitude control system. These errors led to a fatal event: the loss of the solar panels on the Hitomi mission. The X-ray Astronomy Recovery Mission (or, XARM) is proposed to regain the key scientific advances anticipated by the international collaboration behind Hitomi. XARM will recover this science in the shortest time possible by focusing on one of the main science goals of Hitomi,"Resolving astrophysical problems by precise high-resolution X-ray spectroscopy".1This decision was reached after evaluating the performance of the instruments aboard Hitomi and the mission's initial scientific results, and considering the landscape of planned international X-ray astrophysics missions in 2020's and 2030's. Hitomi opened the door to high-resolution spectroscopy in the X-ray universe. It revealed a number of discrepancies between new observational results and prior theoretical predictions. Yet, the resolution pioneered by Hitomi is also the key to answering these and other fundamental questions. The high spectral resolution realized by XARM will not offer mere refinements; rather, it will enable qualitative leaps in astrophysics and plasma physics. XARM has therefore been given a broad scientific charge: "Revealing material circulation and energy transfer in cosmic plasmas and elucidating evolution of cosmic structures and objects". To fulfill this charge, four categories of science objectives that were defined for Hitomi will also be pursued by XARM; these include (1) Structure formation of the Universe and evolution of clusters of galaxies; (2) Circulation history of baryonic matters in the Universe; (3) Transport and circulation of energy in the Universe; (4) New science with unprecedented high resolution X-ray spectroscopy. In order to achieve these scientific objectives, XARM will carry a 6 × 6 pixelized X-ray micro-calorimeter on the focal plane of an X-ray mirror assembly, and an aligned X-ray CCD camera covering the same energy band and a wider field of view. This paper introduces the science objectives, mission concept, and observing plan of XARM.
  DOI：https://doi.org/10.1117/12.2309455
  Scopus Citedby：https://www.scopus.com/inward/citedby.uri?partnerID=HzOxMe3b&scp=85051857277&origin=inward
  DOI ID：10.1117/12.2309455, ISSN：0277-786X, eISSN：1996-756X, SCOPUS ID：85051857277
• X線天文衛星「すざく」搭載広帯域全天モニターWAMによる2005年から2015年までの太陽フレアの観測
  矢部聖也; 田代信; 寺田幸功; 山内誠; 大森法輔; 牧島一夫; 岩切渉; 山岡和貴; 杉田聡司; 深沢泰司; 大野雅功; 河野貴文; 高橋忠幸; 国分紀秀; 中川友進; 浦田裕次; 中澤知洋
  日本天文学会年会講演予稿集, Volume：2016, First page：96, 20 Aug. 2016
  Japanese
  ISSN：1347-0639, J-Global ID：201602246783740824
• In-flight verification of the calibration and performance of the ASTRO-H (Hitomi) Soft X-Ray Spectrometer　　　　　　　　　　　　　　　
  Maurice A. Leutenegger; Marc Audard; Kevin R. Boyce; Gregory V. Brown; Meng P. Chiao; Megan E. Eckart; Ryuichi Fujimoto; Akihiro Furuzawa; Matteo Guainazzi; Daniel Haas; Jan-Willem Den Herder; Takayuki Hayashi; Ryo Iizuka; Manabu Ishida; Yoshitaka Ishisaki; Richard L. Kelley; Naomichi Kikuchi; Caroline A. Kilbourne; Shu Koyama; Sho Kurashima; Yoshitomo Maeda; Maxim Markevitch; Dan McCammon; Kazuhisa Mitsuda; Hideyuki Mori; Nozomi Nakaniwa; Takashi Okajima; Stéphane Paltani; Robert Petre; F. Scott Porter; Kosuke Sato; Toshiki Sato; Makoto Sawada; Peter J. Serlemitsos; Hiromi Seta; Gary Sneiderman; Yang Soong; Satoshi Sugita; Andrew E. Szymkowiak; Yoh Takei; Makoto Tashiro; Yuzuru Tawara; Masahiro Tsujimoto; Cor P. De Vries; Tomomi Watanabe; Shinya Yamada; Noriko Yamasaki
  Proceedings of SPIE - The International Society for Optical Engineering, Volume：9905, 2016, [Reviewed]
  The Soft X-ray Spectrometer (SXS) onboard the Astro-H (Hitomi) orbiting x-ray observatory featured an array of 36 silicon thermistor x-ray calorimeters optimized to perform high spectral resolution x-ray imaging spectroscopy of astrophysical sources in the 0.3-12 keV band. Extensive pre-flight calibration measurements are the basis for our modeling of the pulse-height-energy relation and energy resolution for each pixel and event grade, telescope collecting area, detector efficiency, and pulse arrival time. Because of the early termination of mission operations, we needed to extract the maximum information from observations performed only days into the mission when the onboard calibration sources had not yet been commissioned and the dewar was still coming into thermal equilibrium, so our technique for reconstructing the per-pixel time-dependent pulse-height-energy relation had to be modified. The gain scale was reconstructed using a combination of an absolute energy scale calibration at a single time using a fiducial from an onboard radioactive source, and calibration of a dominant time-dependent gain drift component using a dedicated calibration pixel, as well as a residual time-dependent variation using spectra from the Perseus cluster of galaxies. The energy resolution was also measured using the onboard radioactive sources. It is consistent with instrument-level measurements accounting for the modest increase in noise due to spacecraft systems interference. We use observations of two pulsars to validate our models of the telescope area and detector efficiency, and to derive a more accurate value for the thickness of the gate valve Be window, which had not been opened by the time mission operations ceased. We use observations of the Crab pulsar to refine the pixel-to-pixel timing and validate the absolute timing.
  SPIE, English
  DOI：https://doi.org/10.1117/12.2234230
  DOI ID：10.1117/12.2234230, ISSN：1996-756X, SCOPUS ID：85003422200, Web of Science ID：WOS:000387731500115
• Revolutionize Our Understanding of Time-Domain Astronomy : 10 Years of Swift　　　　　　　　　　　　　　　
  坂本 貴紀; 田代 信; 佐藤 悟朗
  Volume：108, Number：10, First page：642, Last page：655, Oct. 2015
  Japanese
  ISSN：0374-2466, CiNii Articles ID：40020596611, CiNii Books ID：AN00154555
• ASTRO‐H衛星搭載軟ガンマ線検出器の現状と解析ソフトウェアについて
  高橋弘充; 田島宏康; 深沢泰司; 渡辺伸; 渡辺伸; 大野雅功; 北口貴雄; 田中康之; 水野恒史; 太田方之; 小高裕和; 国分紀秀; 佐藤悟朗; 佐藤理江; 武田伸一郎; 林克洋; 原山淳; 森國城; 高橋忠幸; 高橋忠幸; 中澤知洋; 牧島一夫; 田中孝明; 榎戸輝揚; 片岡淳; 谷津陽一; 内山泰伸; 内山秀樹; 中森健之; 山岡和貴; BLANDFORD Roger; MADEJSKI Grzegorz; 田代信; 寺田幸功; 山田真也; 湯浅孝行; 米徳大輔; LAURENT Philippe; LIMOUSIN Olivier; LEBRUN Francois
  日本天文学会年会講演予稿集, Volume：2015, First page：256, 20 Aug. 2015
  Japanese
  ISSN：1347-0639, J-Global ID：201502208558523514
• X-Ray Study of Heavy Element Evolution in Hot Plasmas Associated with Clusters of Galaxies　　　　　　　　　　　　　　　
  下田 優弥; 川原田 円; 田代 信
  Volume：108, Number：4, First page：217, Last page：224, Apr. 2015
  Japanese
  ISSN：0374-2466, CiNii Articles ID：40020404713, CiNii Books ID：AN00154555
• 「すざく」による電波銀河Centaurus AローブのX線観測　　　　　　　　　　　　　　　
  瀬田裕美; 田代信; 井上進
  Volume：2015, 2015
  ISSN：1347-0639, J-Global ID：201502210715909744
• 23pDK-3 Test results of flight models for Soft Gamma-ray Detector on board ASTRO-H　　　　　　　　　　　　　　　
  Tajima Hiroyasu; Blandford Roger; Madejski Grzegorz; Laurent Philippe; Limousin Olivier; Lebrun Francois; SGD team
  Meeting Abstracts of the Physical Society of Japan, Volume：70, First page：470, Last page：470, 2015
  The Physical Society of Japan, Japanese
  DOI：https://doi.org/10.11316/jpsgaiyo.70.1.0_470
  DOI ID：10.11316/jpsgaiyo.70.1.0_470, ISSN：2189-079X, CiNii Articles ID：110009990626, CiNii Books ID：AA12721570
• 25pSJ-3 Results of ight integration test for Soft Gamma-ray Detector on board ASTRO-H　　　　　　　　　　　　　　　
  Hayashi K.; Blandford Roger; Madejski Grzegorz; Laurent Philippe; Limousin Olivier; Lebrun Francois; SGD team
  Meeting Abstracts of the Physical Society of Japan, Volume：70, First page：351, Last page：351, 2015
  The Physical Society of Japan, Japanese
  DOI：https://doi.org/10.11316/jpsgaiyo.70.2.0_351
  DOI ID：10.11316/jpsgaiyo.70.2.0_351, ISSN：2189-079X, CiNii Articles ID：110010028590, CiNii Books ID：AA12721570
• ASTRO‐H衛星搭載軟ガンマ線検出器(SGD)開発の現状
  大野雅功; 田島宏康; 深沢泰司; 渡辺伸; 高橋弘充; 田中康之; 水野恒史; 太田方之; 小高裕和; 川原田円; 国分紀秀; 佐藤理江; 高橋忠幸; 武田伸一郎; 原山淳; 林克洋; 森國城; 湯浅孝行; 佐藤悟朗; 中澤知洋; 野田博文; 牧島一夫; 田中孝明; 榎戸輝揚; 山田真也; 片岡淳; 谷津陽一; 内山泰伸; 内山秀樹; 中森健之; 山岡和貴; BLANDFORD Roger; MADEJSKI Grzegorz; 田代信; 寺田幸功; 米徳大輔; LAURENT Philippe; LIMOUSIN Olivier; LEBRUN Francois
  日本天文学会年会講演予稿集, Volume：2014, First page：276, 20 Feb. 2014
  Japanese
  ISSN：1347-0639, J-Global ID：201402294281184585
• Si/CdTe半導体コンプトンカメラによるsub‐MeV全天観測構想
  中澤知洋; 高橋忠幸; 渡辺伸; 国分紀秀; 一戸悠人; 武田伸一郎; 高島健; 三谷烈史; 田代信; 寺田幸功; 玉川徹; 榎戸輝揚; 能町正治; 羽島宏康; 深沢泰司; 水野恒史; 内山泰伸
  日本天文学会年会講演予稿集, Volume：2014, First page：277, 20 Feb. 2014
  Japanese
  ISSN：1347-0639, J-Global ID：201402231095448228
• 「すざく」による電波銀河Fornax A東ローブのX線観測　　　　　　　　　　　　　　　
  瀬田裕美; 田代信; 井上進
  Volume：2014, 2014
  ISSN：1347-0639, J-Global ID：201402212138756873
• すざく衛星搭載広帯域全天モニタによる太陽フレア観測
  大野雅功; 高木勝俊; 河野貴文; 中村竜; 古井俊也; 深沢泰司; 安田哲也; 石田勇介; 上野遥; 杉本樹信; 遠藤輝; 坂本明弘; 丸谷美恵; 寺田幸功; 田代信; 石川真之介; 大森法輔; 秋山満; 山内誠; 山岡和貴; 杉田聡司; 中川友進; 国分紀秀; 高橋忠幸; 岩切渉; 花畑義隆; 浦田裕次; 中澤知洋; 牧島一夫
  日本天文学会年会講演予稿集, Volume：2013, First page：115, 20 Aug. 2013
  Japanese
  ISSN：1347-0639, J-Global ID：201302239855201540
• 29aBE-2 Constraint on the emission mechanism of short GRBs using its light curve behavior　　　　　　　　　　　　　　　
  Ohno M.; Uehara T.; Hanabata Y.; Kawano T.; Takaki K.; Nakamura R.; Tanaka Y.; Fukazawa Y.; Tashiro M. S.; Yamaoka K.; Sugita S.; Ohmori N.; Suzaku WAM team
  Meeting abstracts of the Physical Society of Japan, Volume：68, Number：1, First page：138, Last page：138, 26 Mar. 2013
  The Physical Society of Japan (JPS), Japanese
  ISSN：1342-8349, CiNii Articles ID：110009642927, CiNii Books ID：AA11439205
• Development of Flight Model for Soft Gamma-ray Detector onboard ASTRO-H　　　　　　　　　　　　　　　
  Tajima Hiroyasu; Blandford Roger; Madejski Grzegorz; Laurent Philippe; Limousin Olivier; Lebrun Frangois; the SGD team
  Meeting Abstracts of the Physical Society of Japan, Volume：68, Number：2, First page：110, Last page：110, 2013
  The Physical Society of Japan, Japanese
  DOI ID：10.11316/jpsgaiyo.68.2.1.0_110_1, ISSN：1342-8349, CiNii Articles ID：110009754521, CiNii Books ID：AA11439205
• 27pBE-5 Development of the Soft Gamma-ray Detector on board ASTRO-H (2^ harf of 2012)　　　　　　　　　　　　　　　
  Mizuno Tsunefumi; Blandford Rogor; Madojski Grzogorz; Laurent Philippe; Limousin Olivier; Lobrun Franoois; SGD team
  Meeting Abstracts of the Physical Society of Japan, Volume：68, Number：1, First page：134, Last page：134, 2013
  The Physical Society of Japan, Japanese
  DOI ID：10.11316/jpsgaiyo.68.1.1.0_134_2, ISSN：1342-8349, CiNii Articles ID：110009642912, CiNii Books ID：AA11439205
• Search for Diffuse X-Rays from the Bow Shock Region of Runaway Star BD+43 3654 with Suzaku　　　　　　　　　　　　　　　
  Yukikatsu Terada; Makoto S. Tashiro; Aya Bamba; Ryo Yamazaki; Tomomi Kouzu; Shu Koyama; Hiromi Seta
  PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN, Volume：64, Number：6, Dec. 2012
  The bow shocks of runaway stars with strong stellar winds of over 2000 km s(-1) can serve as particle acceleration sites. The conversion from stellar wind luminosity into particle acceleration power has an efficiency of the same order of magnitude as those in supernova remnants, based on the radio emission from the bow shock region of runaway star BD +43 3654 (Benaglia et al. 2010, A&A, 517, L10). If this object exhibits typical characteristics, then runaway star systems can contribute a non-negligible fraction of Galactic cosmic-ray electrons. To constrain the maximum energy of accelerated particles from measurements of possible non-thermal emissions in the X-ray band, Suzaku observed BD +43 3654 in 2011 April with an exposure of 99 ks. Because the onboard instruments have a stable and low background level, Suzaku detected a possible enhancement over the background of 7.6 +/- 3.4 counts arcmin(-2) at the bow shock region, where the error represents the 3 a statistics only. However, the excess is not significant within the systematic errors of non-X-ray and cosmic-ray backgrounds of the X-ray Imaging Spectrometer, which are +/- 6.0 and +/- 34 counts arcmin(-2), respectively, and the 3 sigma upper limit in the X-ray luminosity from the shock region, which is 1.1 x 10(32) erg s(-1) per 41.2 arcmin(2) in the 0.5 to 10 keV band. This result leads to three conclusions: (1) a shock-heating process is inefficient on this system; (2) the maximum energy of electrons does not exceed similar to 10 TeV, corresponding to a Lorentz factor of less than 10(7); and (3) the magnetic field in the shock acceleration site might not be as turbulent as those in pulsar wind nebulae and supernova remnants.
  OXFORD UNIV PRESS, English, Technical report
  DOI：https://doi.org/10.1093/pasj/64.6.138
  DOI ID：10.1093/pasj/64.6.138, ISSN：0004-6264, eISSN：2053-051X, arXiv ID：arXiv:1207.5577, Web of Science ID：WOS:000313147700024
• Development of the onboard digital processing system for the soft x-ray spectrometer of ASTRO-H performance in the engineering model tests
  H. Seta; H. Seta; M. S. Tashiro; Y. Ishisaki; M. Tsujimoto; M. Tsujimoto; Y. Shimoda; S. Takeda; S. Yamaguchi; K. Mitsuda; R. Fujimoto; R. Fujimoto; Y. Takei; R. L. Kelley; K. R. Boyce; C. A. Kilborne; C. A. Kilborne; F. S. Porter; J. J. Miko; J. J. Miko; K. Masukawa; K. Matsuda
  Proceedings of SPIE - The International Society for Optical Engineering, Volume：8443, 01 Dec. 2012
  We present the development status of the Pulse Shape Processor (PSP), which is the on-board digital electronics responsible for the signal processing of the X-ray microcalorimeter spectrometer instrument (the Soft X-ray Spectrometer; SXS) for the ASTRO-H satellite planned to be launched in 2014. We finished the design and fabrication for the engineering model, and are currently undertaking a series of performance verification and environmental tests. In this report, we summarize the results obtained in a part of the tests completed in the first half of this year. © 2012 SPIE.
  DOI：https://doi.org/10.1117/12.924638
  DOI ID：10.1117/12.924638, ISSN：0277-786X, SCOPUS ID：84871770829
• ASTRO‐H衛星搭載軟ガンマ線検出器(SGD)の開発現状
  渡辺伸; 田島宏康; 深沢泰司; 太田方之; 小高裕和; 川原田円; 国分紀秀; 佐藤悟朗; 佐藤理江; 高橋忠幸; 武田伸一郎; 森國城; 湯浅孝行; 水野恒史; 高橋弘充; 大野雅功; 内山秀樹; 中澤知洋; 牧島一夫; 田中孝明; 榎戸輝揚; 山田真也; 片岡淳; 中森健之; 谷津陽一; 内山泰伸; BLANDFORD Roger; MADEJSKI Grzegorz; 田代信; 寺田幸功; 米徳大輔; LAURENT Philippe; LIMOUSIN Olivier; LEBRUN Francois
  日本天文学会年会講演予稿集, Volume：2012, First page：275, 20 Aug. 2012
  Japanese
  ISSN：1347-0639, J-Global ID：201202250025785383
• The digital processing system for the soft X-ray spectrometer onboard ASTRO-H the design and the performance
  H. Seta; M. S. Tashiro; Y. Ishisaki; M. Tsujimoto; Y. Shimoda; Y. Abe; T. Yasuda; S. Takeda; M. Asahina; Y. Hiyama; S. Yamaguchi; Y. Terada; K. R. Boyce; F. S. Porter; C. A. Kilbourne; R. L. Kelley; R. Fujimoto; Y. Takei; K. Mitsuda; K. Matsuda; K. Masukawa
  IEEE Transactions on Nuclear Science, Volume：59, First page：366, Last page：372, 01 Apr. 2012
  We report the design and the performance of the engineering model of the digital signal processing system called the Pulse Shape Processor (PSP) for the Soft X-ray Spectrometer (SXS) onboard the ASTRO-H satellite. The SXS employs an X-ray microcalorimeter system, in which X-ray photons are detected as a heat pulse due to photoelectric absorption. The pixelized HgTe absorbers are cooled down to 50 mK. The required energy resolution is 7 eV (FWHM) at 6 keV. Since the data link to the satellite data recorder is limited to 200 kbit s -1, the onboard digital processor PSP plays a critical role in achieving the required resolution. The PSP is also the rate-limiting factor for other performance of the SXS, such as maximum count rate and energy range. In this paper, we show the design of the PSP, and show the performance based on a series of laboratory tests performed with the engineering models of the detector and the analog readout electronics. We found that (1) the PSP can register energy in the 0.07-18 keV band [energy range], (2) the energy resolution of the engineering model system, including the detector, analog electronics, and the PSP, is 4.8-5.7 eV at 5.9 keV [energy resolution], and (3) the PSP has sufficient processing power to handle a point-like source fainter than 0.3 Crab [maximum count rate]. These results are expected to be quite similar to those with the flight model, thus the results will be useful for the observation planning using the SXS. © 2012 IEEE.
  DOI：https://doi.org/10.1109/TNS.2011.2179671
  DOI ID：10.1109/TNS.2011.2179671, ISSN：0018-9499, SCOPUS ID：84859897783
• 26pGJ-8 Development of Soft Gamma-ray Detector onboard ASTRO-H　　　　　　　　　　　　　　　
  Tajima Hiroyasu; Blandford Roger; Madejski Grzegorz; Laurent Philippe; Limousin Olivier; Lebrun Francois
  Meeting Abstracts of the Physical Society of Japan, Volume：67, Number：1, First page：139, Last page：139, 2012
  The Physical Society of Japan, Japanese
  DOI ID：10.11316/jpsgaiyo.67.1.1.0_139_4, ISSN：1342-8349, CiNii Articles ID：110009565334, CiNii Books ID：AA11439205
• 14aSP-9 Developement and Status of the Soft Gamma-ray Detector onboard ASTRO-H　　　　　　　　　　　　　　　
  Fukazawa Y.; Kataoka J.; Kawaharada M.; Kokubun M.; Sato G.; Sato R.; Takahashi T; Takahashi H.; Takeda S.; Tashiro M.; Tanaka T.; Tajima H.; Terada Y.; Nakazawa K.; Nakamori T.; Makishima K.; Mizuno T.; Mori K.; Yatsu Y.; Yamada S.; Yuasa T.; Yonetoku D.; Watanabe S.; Blandford Roger; Madejski Grzegorz; Laurent Philippe; Limousin Olivier; Lebrun Francois; the SGD team; Uchiyama H.; Uchiyama Y.; Enoto T.; Ohta M.; Ohno M.; Odaka H.
  Meeting Abstracts of the Physical Society of Japan, Volume：67, Number：2, First page：119, Last page：119, 2012
  The Physical Society of Japan, Japanese
  DOI ID：10.11316/jpsgaiyo.67.2.1.0_119_1, ISSN：1342-8349, CiNii Articles ID：110009599801, CiNii Books ID：AA11439205
• Development of a digital signal processing system for the X-ray microcalorimeter onboard ASTRO-H (II)
  Y. Shimoda; H. Seta; M. S. Tashiro; Y. Terada; Y. Ishisaki; M. Tsujimoto; K. Mitsuda; T. Yasuda; S. Takeda; Y. Hiyama; K. Masukawa; K. Matsuda; K. R. Boyce
  Journal of Low Temperature Physics, Volume：167, First page：575, Last page：581, 01 Jan. 2012
  The Pulse Shape Processor is a digital signal processing electronics for the microcalorimeter instrument onboard ASTRO-H. Receiving digitized waveform (14 bit, 12.5 kHz sample) from 2×18 channels, two identical units of PSP-A and -B trigger X-ray events, assign five kinds of event grade, and perform optimal filtering to measure energy deposit on the 6 × 6 microcalorimeter pixels. One unit of PSP is composed of one FPGA board and two CPU boards. This paper describes the event processing algorithm to fulfill requirements for the signal processing, and task sharing between FPGA and CPU. © Springer Science+Business Media, LLC 2012.
  DOI：https://doi.org/10.1007/s10909-012-0483-0
  DOI ID：10.1007/s10909-012-0483-0, ISSN：0022-2291, SCOPUS ID：84871778888
• すざく衛星搭載硬X線検出器広帯域全天モニタ部(HXD‐WAM)の現状 IIX
  杉田聡司; 山岡和貴; 深沢泰司; 大野雅功; 高橋拓也; 上原岳士; 花畑義隆; 田代信; 寺田幸功; 岩切渉; 高原一紀; 安田哲也; 中川友進; 高橋忠幸; 国分紀秀; 山内誠; 大森法輔; 秋山満; 牧島一夫; 中澤知洋; VASQUEZ Nicolas; 浦田裕次; TSAI Partick; CHUANG Chia‐Jung; 村上敏夫
  日本天文学会年会講演予稿集, Volume：2011, First page：306, 20 Aug. 2011
  Japanese
  ISSN：1347-0639, J-Global ID：201102206206102257
• 27pGS-6 The status of development of the digital waveform processing system PSP in the soft X-ray spectrometer SXS onboard ASTRO-H　　　　　　　　　　　　　　　
  Shimoda Y.; Seta H.; Tashiro M.; Terada Y.; Yasuda T.; Takeda S.; Ishisaki Y.; Abe Y.; Tsujimoto M.; Mitsuda K.; Boyce Kevin; Matsuda K.; Masukawa K.
  Meeting abstracts of the Physical Society of Japan, Volume：66, Number：1, First page：121, Last page：121, 03 Mar. 2011
  The Physical Society of Japan (JPS), Japanese
  ISSN：1342-8349, CiNii Articles ID：110008610164, CiNii Books ID：AA11439205
• 27pGS-7 Quantitivity of timing accuracy in the time distribution system on board ASTRO-H (2)　　　　　　　　　　　　　　　
  Kouzu T.; Iwase K.; Terada Y.; Mishima Y.; Tashiro M. S.; Ishisaki Y.; Yuasa T.; Nomachi M.; Takahashi T.; Kokubun M.; Ozaki M.; ASTRO-H collaborations
  Meeting abstracts of the Physical Society of Japan, Volume：66, Number：1, First page：121, Last page：121, 03 Mar. 2011
  The Physical Society of Japan (JPS), Japanese
  ISSN：1342-8349, CiNii Articles ID：110008610165, CiNii Books ID：AA11439205
• ASTRO‐H衛星搭載軟ガンマ線検出器(SGD)の開発の現状　　　　　　　　　　　　　　　
  田中孝明; 内山泰伸; 榎戸輝揚; 太田方之; 大野雅功; 片岡淳; 川原田円; 国分紀秀; 佐藤悟朗; 高橋忠幸; 高橋弘充; 田島宏康; 田代信; 寺田幸功; 中澤知洋; 中森健之; 深沢泰司; BLANDFORD Roger; 牧島一夫; MADEJSKI Grzegorz; 水野恒史; 森國城; 谷津陽一; 山岡和貴; LAURENT Philippe; LIMOUSIN Olivier; LEBRUN Francois; 渡辺伸
  日本物理学会講演概要集, Volume：66, Number：1, First page：122, Last page：122, 03 Mar. 2011
  The Physical Society of Japan (JPS), Japanese
  ISSN：1342-8349, J-Global ID：201102200104808572, CiNii Articles ID：110008610166, CiNii Books ID：AA11439205
• ASTRO‐H衛星硬X線・軟ガンマ線検出器アクティブシールドの構造設計　　　　　　　　　　　　　　　
  中島健太; 中野俊男; 中澤知洋; 牧島一夫; 花畑義隆; 深沢泰司; 山岡和貴; 田島宏康; 片岡淳; 高橋弘充; 水野恒史; 大野雅功; 国分紀秀; 高橋忠幸; 渡辺伸; 田代信; 寺田幸功
  日本物理学会講演概要集, Volume：66, Number：1, First page：122, Last page：122, 03 Mar. 2011
  The Physical Society of Japan (JPS), Japanese
  ISSN：1342-8349, J-Global ID：201102253748599164, CiNii Articles ID：110008610169, CiNii Books ID：AA11439205
• 18pSX-7 Developments of Soft Gamma-ray Detector on board the ASTRO-H satellite　　　　　　　　　　　　　　　
  Watanabe Shin; Kataoka Jun; Kawaharada Madoka; Kokubun Motohide; Sato Goro; Takahashi Hiromitsu; Takahashi Tadayuki; Tashiro Makoto; Tanaka Takaaki; Terada Yukikatsu; Nakazawa Kazuhiro; Tajima Hiroyasu; Nakamori Takeshi; Blandford Roger; Makishima Kazuo; Madeiski Grzegorz; Mizuno Tsunefumi; Mori Kunishiro; Yatsu Yoichi; Yuasa Takayuki; Laurent Philippe; Limousin Olivier; Fukazawa Yasushi; Lebrun Francois; ASTRO-H SGD team; Uchiyama Hideki; Uchiyama Yasunobu; Enoto Teruaki; Ohta Masayuki; Ohno Masanori; Odaka Hirokazu
  Meeting Abstracts of the Physical Society of Japan, Volume：66, Number：2, First page：112, Last page：112, 2011
  The Physical Society of Japan, Japanese
  DOI ID：10.11316/jpsgaiyo.66.2.1.0_112_4, ISSN：1342-8349, CiNii Articles ID：110008757637, CiNii Books ID：AA11439205
• 26aGS-8 Suzaku observation of black hole candidate XTE J1752-223　　　　　　　　　　　　　　　
  Koyama S; Tashiro M. S; Terada Y; Seta H; Kubota A; Yamaoka K
  Meeting Abstracts of the Physical Society of Japan, Volume：66, Number：0, First page：110, Last page：110, 2011
  一般社団法人 日本物理学会, Japanese
  ISSN：1342-8349, CiNii Articles ID：110008610124, CiNii Books ID：AA11439205
• ASTRO‐H衛星硬X線・軟ガンマ線検出器アクティブシールドの機構開発
  中島健太; 中澤知洋; 中野俊男; 西岡博之; 牧島一夫; 花畑義隆; 高橋弘充; 水野恒史; 深沢泰司; 山岡和貴; 田島宏康; 片岡淳; 大野雅功; 国分紀秀; 高橋忠幸; 渡辺伸; 田代信; 寺田幸功
  日本天文学会年会講演予稿集, Volume：2010, First page：226, 20 Aug. 2010
  Japanese
  ISSN：1347-0639, J-Global ID：201002297490938422
• 20aBP-7 Quantitivity of timing accuracy in the time distribution system on board ASTRO-H　　　　　　　　　　　　　　　
  Kouzu T.; Terada Y.; Tashiro M. S.; Iwase K.; Yuasa T.; Nomachi M.; Ishisaki Y.; Takahashi T.; Kokubun M.; Ozaki M.; ASTRO-H collaborations
  Meeting abstracts of the Physical Society of Japan, Volume：65, Number：1, First page：103, Last page：103, 01 Mar. 2010
  The Physical Society of Japan (JPS), Japanese
  ISSN：1342-8349, CiNii Articles ID：110007654192, CiNii Books ID：AA11439205
• ASTRO‐H衛星搭載硬X線・軟ガンマ線検出器アクティブシールドの開発(I):光読み出し　　　　　　　　　　　　　　　
  花畑義隆; 深沢泰司; 山岡和貴; 田島宏康; 片岡淳; 中澤知洋; 高橋弘充; 水野恒史; 大野雅功; 国分紀秀; 高橋忠幸; 渡辺伸; 田代信; 寺田幸功; 佐々木智香子; 中島健太; 水島翼
  日本物理学会講演概要集, Volume：65, Number：1, First page：103, Last page：103, 01 Mar. 2010
  The Physical Society of Japan (JPS), Japanese
  ISSN：1342-8349, J-Global ID：201002201347165644, CiNii Articles ID：110007654193, CiNii Books ID：AA11439205
• ASTRO‐H衛星硬X線・軟ガンマ線検出器アクティブシールドの開発(II):機構開発
  中島健太; 中澤知洋; 西岡博之; 牧島一夫; 花畑義隆; 深沢泰司; 山崎和貴; 田島宏康; 片岡淳; 高橋弘充; 水野恒史; 大野雅功; 国分紀秀; 高橋忠幸; 渡辺伸; 田代信; 寺田幸功; 佐々木智香子; 水島翼
  日本物理学会講演概要集, Volume：65, Number：1, First page：103, 01 Mar. 2010
  Japanese
  ISSN：1342-8349, J-Global ID：201002297783303073
• 「すざく」衛星搭載硬X線検出器広帯域全天モニタ部(HXD‐WAM)の現状(IX)
  山岡和貴; 田代信; 寺田幸功; 恩田香織; 遠藤輝; 岩切渉; 菅佐原たか子; 大野雅功; 鈴木素子; 国分紀秀; 高橋忠幸; 杉田聡司; 深沢泰司; 高橋拓也; 上原岳士; 花畑義隆; 山内誠; 園田絵里; 大森法輔; 河野健太; 林秀憲; 野田和宏; 大休寺新; 西岡祐介; 中澤知洋; 榎戸輝揚; 牧島一夫; 玉川徹; 中川友進; 浦田裕次; 林紅妙; VASQUEZ Nicolas; 洪秀徴; 村上敏夫; 田島宏康
  日本天文学会年会講演予稿集, Volume：2010, First page：264, 20 Feb. 2010
  Japanese
  ISSN：1347-0639, J-Global ID：201002225747874004
• 「すざく」衛星搭載WAM検出器による太陽フレアに伴う硬X線の系統的解析　　　　　　　　　　　　　　　
  遠藤輝; 嶋森篤史; 田代信; 寺田幸功; 浦田裕次; 浦田裕次; 園田絵里; 山内誠; 山岡和貴; 深沢泰司; 大野雅功; 渡邉恭子; 杉田聡司; 簑島敬
  Volume：2010, 2010
  ISSN：1347-0639, J-Global ID：201002270585130109
• Development of a digital signal processing system for the X-ray microcalorimeter onboard ASTRO-H
  Hiromi Seta; Makoto S. Tashiro; Yukikatsu Terada; Yuya Shimoda; Kaori Onda; Yoshitaka Ishisaki; Masahiro Tsujimoto; Toshishige Hagihara; Yoh Takei; Kazuhisa Mitsuda; Kevin R. Boyce; Andrew E. Szymkowiak
  AIP Conference Proceedings, Volume：1185, First page：278, Last page：281, 01 Dec. 2009
  A digital signal processing system for the X-ray microcalorimeter array (SXS) is being developed for the next Japanese X-ray astronomy satellite, ASTRO-H. The SXS digital signal processing system evaluates each pulse by an optimal filtering process. For the ASTRO-H project, we decided to employ digital electronics hardware, which includes a digital I/O board based upon FPGAs, and a separate CPU board. It is crucially important for the FPGA to be able to detect the presence of an "secondary" pulses on the tail of an initial pulse. In order to detect the contaminating pulses, we have developed a new finite impulse response filter, to compensate for the undershoot in the derivative. By employing the filter it is possible for FPGA to detect the secondary pulse very close the first pulse, and to reduce the load of the CPU in the secondary pulse searching process. © 2009 American Institute of Physics.
  DOI：https://doi.org/10.1063/1.3292332
  DOI ID：10.1063/1.3292332, ISSN：0094-243X, SCOPUS ID：74349129999
• SUZAKU OBSERVATION OF THE GIANT RADIO GALAXY 3C 326　　　　　　　　　　　　　　　
  Naoki Isobe; Makoto S. Tashiro; Poshak Gandhi; Asami Hayato; Hiroshi Nagai; Kazuhiro Hada; Hiromi Seta; Keiko Matsuta
  ASTROPHYSICAL JOURNAL, Volume：706, Number：1, First page：454, Last page：463, Nov. 2009
  A Suzaku observation of a giant radio galaxy, 3C 326, which has a physical size of about 2 Mpc, was conducted on 2008 January 19-21. In addition to several X-ray sources, diffuse emission was significantly detected and associated with its west lobe, but the east lobe was contaminated by an unidentified X-ray source WARP J1552.4+2007. After careful evaluation of the X-ray and non-X-ray background, the 0.4-7 keV X-ray spectrum of the west lobe is described by a power-law model modified with the Galactic absorption. The photon index and 1 keV flux density were derived as Gamma = 1.82(-0.24)(+0.26) +/- 0.04 and S-X = 19.4(-3.2)(+3.3) +/- 3.0 nJy, respectively, where the first and second errors represent the statistical and systematic ones. The diffuse X-rays were attributed to be inverse Compton (IC) radiation by the synchrotron radio electrons scattering off the cosmic microwave background photons. This radio galaxy is the largest among those with lobes detected through IC X-ray emission. A comparison of the radio to X-ray fluxes yields the energy densities of electron and magnetic field as u(e) = (2.3 +/- 0.3 +/- 0.3) x 10(-13) erg cm(-3) and u(m) = (1.2(-0.1)(+0.2) +/- 0.2) x 10(-14) erg cm(-3), respectively. The galaxy is suggested to host a low-luminosity nucleus with an absorption-corrected 2-10 keV luminosity of < 2 x 10(42) erg s(-1), together with a relatively weak radio core. The energetics in the west lobe of 3C 326 were compared with those of moderate radio galaxies with a size of similar to 100 kpc. The west lobe of 3C 326 is confirmed to agree with the correlations for the moderate radio galaxies, u(e) proportional to D-2.2 +/- 0.4 and u(m) proportional to D-2.4 +/- 0.4, where D is their total physical size. This implies that the lobes of 3C 326 are still being energized by the jet, despite the current weakness of the nuclear activity.
  IOP PUBLISHING LTD, English, Technical report
  DOI：https://doi.org/10.1088/0004-637X/706/1/454
  DOI ID：10.1088/0004-637X/706/1/454, ISSN：0004-637X, eISSN：1538-4357, arXiv ID：arXiv:0910.2467, Web of Science ID：WOS:000271538900035
• TESTING THE E-peak-E-iso RELATION FOR GRBs DETECTED BY SWIFT AND SUZAKU-WAM　　　　　　　　　　　　　　　
  H. A. Krimm; K. Yamaoka; S. Sugita; M. Ohno; T. Sakamoto; S. D. Barthelmy; N. Gehrels; R. Hara; J. P. Norris; N. Ohmori; K. Onda; G. Sato; H. Tanaka; M. Tashiro; M. Yamauchi
  ASTROPHYSICAL JOURNAL, Volume：704, Number：2, First page：1405, Last page：1432, Oct. 2009
  One of the most prominent, yet controversial associations derived from the ensemble of prompt-phase observations of gamma-ray bursts (GRBs) is the apparent correlation in the source frame between the peak energy (E-peak) of the nu F(nu) spectrum and the isotropic radiated energy, E-iso. Since most GRBs have E-peak above the energy range (15-150 keV) of the Burst Alert Telescope (BAT) on Swift, determining accurate E-peak values for large numbers of Swift bursts has been difficult. However, by combining data from Swift/BAT and the Suzaku Wideband All-Sky Monitor (WAM), which covers the energy range from 50 to 5000 keV, for bursts which are simultaneously detected, one can accurately fit E-peak and E-iso and test the relationship between them for the Swift sample. Between the launch of Suzaku in 2005 July and the end of 2009 April, there were 48 GRBs that triggered both Swift/BAT and WAM, and an additional 48 bursts that triggered Swift and were detected by WAM, but did not trigger. A BAT-WAM team has cross-calibrated the two instruments using GRBs, and we are now able to perform joint fits on these bursts to determine their spectral parameters. For those bursts with spectroscopic redshifts, we can also calculate the isotropic energy. Here, we present the results of joint Swift/BAT-Suzaku/WAM spectral fits for 91 of the bursts detected by the two instruments. We show that the distribution of spectral fit parameters is consistent with distributions from earlier missions and confirm that Swift bursts are consistent with earlier reported relationships between E-peak and isotropic energy. We show through time-resolved spectroscopy that individual burst pulses are also consistent with this relationship.
  IOP PUBLISHING LTD, English, Book review
  DOI：https://doi.org/10.1088/0004-637X/704/2/1405
  DOI ID：10.1088/0004-637X/704/2/1405, ISSN：0004-637X, eISSN：1538-4357, Web of Science ID：WOS:000270486200032
• 「すざく」衛星搭載硬X線検出器広帯域全天モニタ部(HXD‐WAM)の現状(VIII)
  田代信; 寺田幸功; 恩田香織; 遠藤輝; 岩切渉; 菅佐原たか子; 大野雅功; 鈴木素子; 国分紀秀; 高橋忠幸; 山岡和貴; 杉田聡司; 深沢泰司; 上原岳士; 花畑義隆; 山内誠; 園田絵里; 大森法輔; 河野健太; 林秀憲; 野田和宏; 大休寺新; 西岡祐介; 中澤知洋; 榎戸輝揚; 牧島一夫; 玉川徹; 中川友進; 浦田裕次; VASQUEZ Nicolas; 洪秀徴; 田島宏康
  日本天文学会年会講演予稿集, Volume：2009, First page：263, 20 Aug. 2009
  Japanese
  ISSN：1347-0639, J-Global ID：200902237947430132
• 10aSD-11 Development status of the Soft X-ray Spectrometer (SXS) onboard Astro-H (II)　　　　　　　　　　　　　　　
  Fujimoto Ryuichi; Sato Kosuke; Mitsuda Kazuhisa; Yamasaki Noriko; Takei Yoh; Tsujimoto Masahiro; Sugita Hiroyuki; Sato Yoichi; Shinozaki Keisuke; Ohashi Takaya; Ishisaki Yoshitaka; Ezoe Yuichiro; Murakami Masahide; Tashiro Makoto; Terada Yukikatsu; Tamagawa Toru; Mihara Tatehiro; Kawaharada Madoka; Yamaguchi Hiroya; Kitamoto Shunji; Murakami Hiroshi; Kelley R.L; Kilbourne C.A; Porter F.S; McCammon D; den Herder J.-W
  Meeting abstracts of the Physical Society of Japan, Volume：64, Number：2, First page：31, Last page：31, 18 Aug. 2009
  The Physical Society of Japan (JPS), Japanese
  ISSN：1342-8349, CiNii Articles ID：110007501526, CiNii Books ID：AA11439205
• Time-Evolution of Peak Energy and Luminosity Relation within Pulses for GRB 061007: Probing Fireball Dynamics　　　　　　　　　　　　　　　
  Masanori Ohno; Kunihito Ioka; Kazutaka Yamaoka; Makoto Tashiro; Yasushi Fukazawa; Yujin E. Nakagawa
  PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN, Volume：61, Number：2, First page：201, Last page：211, Apr. 2009
  We performed a time-resolved spectral analysis of a bright, long gamma-ray burst GRB 061007 using Suzaku/WAM and Swift/BAT. Because of the large effective area of the WAM, we can investigate the time evolution of the spectral peak energy E-peak(t) and the luminosity L-iso(t) with 1-s time resolution, and we find that the time-resolved pulses also satisfy the E-peak-L-iso relation, which was found for the time-averaged spectra of other bursts, suggesting the same physical conditions in each pulse. Furthermore, the initial rising phase of each pulse could be an outlier of this relation with higher E-peak(t) Value by a factor of 2. This difference could Suggest that the fireball radius expands by a factor of 2-4 and / or bulk Lorentz factor of the fireball is decelerated by a factor of similar to 4 during the initial phase, providing a new probe of fireball dynamics in real time.
  OXFORD UNIV PRESS, English
  DOI：https://doi.org/10.1093/pasj/61.2.201
  DOI ID：10.1093/pasj/61.2.201, ISSN：0004-6264, eISSN：2053-051X, Web of Science ID：WOS:000266228300006
• 28pSH-1 Prompt emission and X-ray afterglow observations of GRB070328 with Suzaku and Swift　　　　　　　　　　　　　　　
  Henmi Kaori; Tashiro Makoto; Onda Kaori; Iwakiri Wataru; Nakagawa Yujin; Yamauchi Makoto; Hara Ryuji; Nishioka Yusuke; Murakami Toshio; Yonetoku Daisuke; Emura Naomi; Suzaku ToO Team; Suzaku WAM Team
  Meeting abstracts of the Physical Society of Japan, Volume：64, Number：1, First page：92, Last page：92, 03 Mar. 2009
  The Physical Society of Japan (JPS), Japanese
  ISSN：1342-8349, CiNii Articles ID：110007370068, CiNii Books ID：AA11439205
• 28pSH-6 Development of the signal processing system for the X-ray microcalorimeter onboard ASTRO-H　　　　　　　　　　　　　　　
  Seta Hiromi; Tashiro Makoto; Terada Yukikatsu; Onda Kaori; Shimoda Yuuya; Ishisaki Yoshitaka; Takei Yoh; Mitsuda Kazuhisa; ASTRO-H SXS team
  Meeting abstracts of the Physical Society of Japan, Volume：64, Number：1, First page：93, Last page：93, 03 Mar. 2009
  The Physical Society of Japan (JPS), Japanese
  ISSN：1342-8349, CiNii Articles ID：110007370071, CiNii Books ID：AA11439205
• 28pSH-5 Development of mirocalorimeter SXS designed for ASTRO-H　　　　　　　　　　　　　　　
  Takei Y; Mitsuda K; Yamasaki N; Tsujimoto M; Shinozaki K; Sugita H; Sato Y; Fujimoto R; Sato K; Ohashi T; Ishisaki Y; Ezoe Y; Murakami M; Tashiro M. S; Terada Y; Tamagawa T; Mihara T; Kawaharada M; Yamaguchi H; Kitamoto S; Murakami H; Kelley Richard L; Kilbourne C. A; Porter F. S; Shirron P. J; DiPirro M. J; Sneiderman Gary A; McCammon D; Herder J.-W. den; ASTRO-H SXS tea
  Meeting abstracts of the Physical Society of Japan, Volume：64, Number：1, First page：92, Last page：92, 03 Mar. 2009
  The Physical Society of Japan (JPS), Japanese
  ISSN：1342-8349, CiNii Articles ID：110007370070, CiNii Books ID：AA11439205
• 「すざく」衛星搭載硬X線検出器広帯域全天モニタ部(HXD‐WAM)の現状(VII)
  大野雅功; 国分紀秀; 鈴木素子; 高橋忠幸; 田代信; 寺田幸功; 浦田裕次; 恩田香織; 遠藤輝; 小高夏来; 守上浩市; 岩切渉; 菅佐原たか子; 山岡和貴; 杉田聡司; 玉川徹; 中川友進; 深沢泰司; 高橋拓也; 上原岳士; 吉良知恵; 花畑義隆; 中澤知洋; 榎戸輝揚; 牧島一夫; 洪秀徴; 山内誠; 園田絵里; 田中裕基; 原龍児; 大森法輔; 河野健太; 林秀憲; 田島宏康
  日本天文学会年会講演予稿集, Volume：2009, First page：253, 20 Feb. 2009
  Japanese
  ISSN：1347-0639, J-Global ID：200902296985521636
• Time-Evolution of Peak Energy and Luminosity Relation within Pulses for GRB 061007: Probing Fireball Dynamics　　　　　　　　　　　　　　　
  M. Ohno; K. Ioka; K. Yamaoka; M. Tashiro; Y. Fukazawa; Y. E. Nakagawa
  Volume：61, Number：2, First page：201, Last page：211, 2009
• Suzaku Observations of SGR 1900+14 and SGR 1806-20　　　　　　　　　　　　　　　
  Yujin E. Nakagawa; Tatehiro Mihara; Atsumasa Yoshida; Kazutaka Yamaoka; Satoshi Sugita; Toshio Murakami; Daisuke Yonetoku; Motoko Suzuki; Motoki Nakajima; Makoto S. Tashiro; Kazuhiro Nakazawa
  PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN, Volume：61, First page：S387, Last page：S393, Jan. 2009
  Spectral and timing studies of Suzaku ToO observations of two SGRs, 1900+14 and 1806-20, are presented. The X-ray quiescent emission spectra were well fitted by a two blackbody function, or a blackbody plus a power-law model. The non-thermal hard component discovered by INTEGRAL was detected by PIN diodes and its spectrum was reproduced by the power-law model reported by INTEGRAL. The XIS detected a periodicity of P = 5.1998 +/- 0.0002s for SGR 1900+14 and P = 7.6022 +/- 0.0007s for SGR 1806-20. The pulsed fraction was related to the burst activity for SGR 1900+14.
  OXFORD UNIV PRESS, English
  DOI：https://doi.org/10.1093/pasj/61.sp1.S387
  DOI ID：10.1093/pasj/61.sp1.S387, ISSN：0004-6264, eISSN：2053-051X, Web of Science ID：WOS:000264418100037
• Hard X-Ray Spectrum from West Lobe of Radio Galaxy Fornax A Observed with Suzaku　　　　　　　　　　　　　　　
  Makoto S. Tashiro; Naoki Isobe; Hiromi Seta; Keiko Matsuta; Yuichi Yaji
  PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN, Volume：61, First page：S327, Last page：S335, Jan. 2009
  An observation of the West lobe of radio galaxy Fornax A (NGC 1316) with Suzaku is reported. Since Feigelson et al. (1995, ApJ, 449, L149) and Kaneda et al.(1995, AN, 453, L13) discovered the cosmic microwave background boosted inverse-Comptonized (IC) X-rays from the radio lobe, the magnetic field and electron energy density in the lobes have been estimated under the assumption that a single component of the relativistic electrons generates both the IC X-rays and the synchrotron radio emission. However, electrons generating the observed IC X-rays in the 1-10 keV band do not possess sufficient energy to radiate the observed synchrotron radio emission under the estimated magnetic field of a few mu G. On the basis of observations made with Suzaku, we show in the present paper that a 0.7-20 keV spectrum is well described by a single power-law model with an energy index of 0.68 and a flux density of 0.12 +/- 0.01 nJy at 1 keV from the West lobe. The derived multiwavelength spectrum strongly suggests that a single electron energy distribution over a Lorentz factor gamma = 300-90000 is responsible for generating both the X-ray and radio emissions. The derived physical quantities are not only consistent with those reported for the West lobe, but are also in very good agreement with those reported for the East lobe.
  OXFORD UNIV PRESS, English
  DOI：https://doi.org/10.1093/pasj/61.sp1.S327
  DOI ID：10.1093/pasj/61.sp1.S327, ISSN：0004-6264, eISSN：2053-051X, Web of Science ID：WOS:000264418100032
• OBSERVATIONS OF THE PROMPT GAMMA-RAY EMISSION OF GRB 070125　　　　　　　　　　　　　　　
  Eric C. Bellm; Kevin Hurley; Valentin Pal'shin; Kazutaka Yamaoka; Mark S. Bandstra; Steven E. Boggs; Soojing Hong; Natsuki Kodaka; A. S. Kozyrev; M. L. Litvak; I. G. Mitrofanov; Yujin E. Nakagawa; Masanori Ohno; Kaori Onda; A. B. Sanin; Satoshi Sugita; Makoto Tashiro; V. I. Tretyakov; Yuji Urata; Claudia Wigger
  ASTROPHYSICAL JOURNAL, Volume：688, Number：1, First page：491, Last page：498, Nov. 2008
  The long, bright gamma-ray burst GRB 070125 was localized by the Interplanetary Network. We present light curves of the prompt gamma-ray emission as observed by Konus-Wind, RHESSI, Suzaku WAM, and Swift BAT. We detail the results of joint spectral fits with Konus and RHESSI data. The burst shows moderate hard-to-soft evolution in its multipeaked emission over a period of about 1 minute. The total burst fluence as observed by Konus is 1: 79; 10(-4) ergs cm(-2) (20 keV-10 MeV). Using the spectroscopic redshift z = 1.548, we find that the burst is consistent with the "Amati'' E-peak,(i)-E-iso correlation. Assuming a jet opening angle derived from broadband modeling of the burst afterglow, GRB 070125 is a significant outlier to the "Ghirlanda'' E-peak,(i)-E-gamma correlation. Its collimation-corrected energy release, E-gamma = 2.5 x 10(52) ergs, is the largest yet observed.
  UNIV CHICAGO PRESS, English
  DOI：https://doi.org/10.1086/592136
  DOI ID：10.1086/592136, ISSN：0004-637X, Web of Science ID：WOS:000260769700039
• 22pSH-4 Soft gamma-ray long-term earth occultation observations of black hole sources with Suzaku-WAM　　　　　　　　　　　　　　　
  Kira Chie; Fukazawa Yasushi; Takahashi Hiromitsu; Takahashi Takuya; Uehara Takeshi; Hanabata Yoshitaka; Yamaoka Kazuki; Tashiro Makoto; Ohno Masanori; Tamagawa Tohru; Terada Yukinori
  Meeting abstracts of the Physical Society of Japan, Volume：63, Number：2, First page：89, Last page：89, 25 Aug. 2008
  The Physical Society of Japan (JPS), Japanese
  ISSN：1342-8349, CiNii Articles ID：110006982710, CiNii Books ID：AA11439205
• 「すざく」衛星による軟ガンマ線リピータSGR1900+14/1806‐20の観測
  中川友進; 三原建弘; 吉田篤正; 山岡和貴; 杉田聡司; 鈴木素子; 中島基樹; 村上敏夫; 米徳大介; 田代信; 中澤知洋
  日本天文学会年会講演予稿集, Volume：2008, First page：98, 20 Aug. 2008
  Japanese
  ISSN：1347-0639, J-Global ID：200902243657841392
• すざく衛星搭載WAMによるガンマ線バーストの広帯域高感度観測
  大野雅功; 国分紀秀; 鈴木素子; 高橋忠幸; 山岡和貴; 杉田聡司; 田代信; 寺田幸功; 浦田裕次; 恩田香織; 遠藤輝; 鈴木正信; 小高夏来; 守上浩市; 岩切渉; 菅佐原たか子; 玉川徹; 中川友進; 深沢泰司; 高橋拓也; 上原岳士; 吉良知恵; 花畑義隆; 中澤知洋; 榎戸輝揚; 牧島一夫; 洪秀徴; 山内誠; 園田絵里; 田中裕基; 原龍児; 大森法輔; 田島宏康
  日本天文学会年会講演予稿集, Volume：2008, First page：75, 20 Aug. 2008
  Japanese
  ISSN：1347-0639, J-Global ID：200902270078743858
• 「すざく」衛星による2006年12月5日のX9太陽フレアからの中性子検出の可能性 II　　　　　　　　　　　　　　　
  北口貴雄; 江戸輝揚; 中澤知洋; 牧島一夫; 馬場彩; 国分紀秀; 川原田円; 遠藤輝; 浦田裕次; 寺田幸功; 田代信; 山岡和貴; HONG S; 土屋晴文; LOEWENSTEIN Michael
  日本物理学会講演概要集, Volume：63, Number：1, First page：105, Last page：105, 29 Feb. 2008
  The Physical Society of Japan (JPS), Japanese
  ISSN：1342-8349, J-Global ID：200902239349446957, CiNii Articles ID：110007144101, CiNii Books ID：AA11439205
• Spectral properties of prompt emission of four short gamma-ray bursts observed by the Suzaku-WAM and the Konus-wind　　　　　　　　　　　　　　　
  Masanori Ohno; Yasushi Fukazawa; Takuya Takahashi; Kazutaka Yamaoka; Satoshi Sugita; Valentin Pal'shin; Dmitry Frederiks; Philipp Oleynik; Mikhail Ulanov; Takanori Sakamoto; Goro Sato; Kevin Hurley; Makoto S. Tashiro; Yuji Urata; Kaori Onda; Toru Tamagawa; Yukikatsu Terada; Motoko Suzuki; Hong Soojing
  PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN, Volume：60, First page：S361, Last page：S373, Feb. 2008
  We have performed a joint analysis of prompt emission from four bright short gamma-ray bursts (GRBs) with the Suzaku-WAM and the Konus-Wind experiments. This joint analysis allows us to investigate the spectral properties of short-duration bursts over a wider energy band with a higher accuracy. We find that these bursts have a high E-peak, around 1 MeV and have a harder power-law component than that of long GRBs. However, we can not determine whether these spectra follow the cut-off power-law model or the Band model. We also investigated the spectral lag, hardness ratio, inferred isotropic radiation energy and existence of a soft emission hump, in order to classify them into short or long GRBs using several criteria, in addition to the burst duration. We find that all criteria, except for the existence of the soft hump, support the fact that our four GRB samples are correctly classified as belonging to the short class. In addition, our broad-band analysis revealed that there is no evidence of GRBs with a very large hardness ratio, as seen in the BATSE short GRB sample, and that the spectral lag of our four short GRBs is consistent with zero, even in the MeV energy band, unlike long GRBs. Although our short GRB samples are still limited, these results suggest that the spectral hardness of short GRBs might not differ significantly from that of long GRBs, and also that the spectral lag at high energies could be a strong criterion for burst classification.
  OXFORD UNIV PRESS, English
  DOI：https://doi.org/10.1093/pasj/60.sp1.S361
  DOI ID：10.1093/pasj/60.sp1.S361, ISSN：0004-6264, eISSN：2053-051X, Web of Science ID：WOS:000255818700035
• Spectral evolution of GRB 060904A observed with swift and Suzaku - Possibility of inefficient electron acceleration　　　　　　　　　　　　　　　
  Daisuke Yonetoku; Sachiko Tanabe; Toshio Murakami; Naomi Emura; Yuka Aoyama; Takashi Kidamura; Hironobu Kodaira; Yoshiki Kodama; Ryota Kozaka; Takuro Nashimoto; Shinya Okuno; Satoshi Yokota; Satoru Yoshinari; Keiichi Abe; Kaori Onda; Makoto S. Tashiro; Yuji Urata; Yujin E. Nakagawa; Satoshi Sugita; Kazutaka Yamaoka; Atsumasa Yoshida; Takuto Ishimura; Nobuyuki Kawai; Takashi Shimokawabe; Kenzo Kinugasa; Takayoshi Kohmura; Kaori Kubota; Kei Sugiyasu; Yoshihiro Ueda; Kensuke Masui; Kazuhiro Nakazawa; Tadayuki Takahashi; Shouta Maeno; Eri Sonoda; Makoto Yamauchi; Makoto Kuwahara; Toru Tamagawa; Daisuke Matsuura; Motoko Suzuki; Scott Barthelmy; Neil Gehrels; John Nousek
  PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN, Volume：60, First page：S351, Last page：S360, Feb. 2008
  We observed an X-ray afterglow of GRB 060904A with the Swift and Suzaku satellites. We found rapid spectral softening during both the prompt tail phase and the decline phase of an X-ray flare in the Swift/BAT and Swift/XRT +004 data. The observed spectra were fit by power-law photon indices which rapidly changed from Gamma = (+1.51)(-0.03) to Gamma = 5.30(-0.59)(+0.69) within a few hundred seconds. This is one of the steepest X-ray spectra ever observed, making it quite difficult to explain by simple electron-acceleration and synchrotron -radiation processes. We then applied an alternative broken power-law with exponential cutoff (BPEC) model. It is valid to consider the exponential shape is equivalent to a synchrotron cutoff. Since the spectral cutoff appears in the soft X-ray band, we conclude that the electron acceleration must be inefficient in the internal shocks of GRB 060904A. These cutoff spectra suddenly disappeared at the end of the prompt tail. After that, typical afterglow spectra with F = 2.0 have been continuously and preciously monitored by both Swift/XRT and Suzaku/XIS. We could successfully trace the temporal history of two characteristic break energies that have a time dependence of (proportional to t(-3)-t(-4), while the following afterglow spectra are quite stable. This fact indicates that the emitting material of the prompt tail is due to completely different dynamics from the shallow decay component. Therefore, the emission sites of two distinct phenomena obviously differ from each other.
  OXFORD UNIV PRESS, English
  DOI：https://doi.org/10.1093/pasj/60.sp1.S351
  DOI ID：10.1093/pasj/60.sp1.S351, ISSN：0004-6264, eISSN：2053-051X, Web of Science ID：WOS:000255818700034
• In-orbit timing calibration of the hard X-ray detector on board Suzaku　　　　　　　　　　　　　　　
  Yukikatsu Terada; Teruaki Enoto; Ryouhei Miyawaki; Yoshitaka Ishisaki; Tadayasu Dotani; Ken Ebisawa; Masanobu Ozaki; Yoshihiro Ueda; Lucien Kuiper; Manabu Endo; Yasushi Fukazawa; Tsuneyoshi Kamae; Madoka Kawaharada; Motohide Kokubun; Yoshikatsu Kuroda; Kazuo Makishinia; Kazunori Masukawa; Tsunefumi Mizuno; Toshio Murakami; Kazuhiro Nakazawa; Atsushi Nakajima; Masaharu Nomach; Naoki Shibayama; Tadayuki Takahash; Hiromitsu Takahashi; Makoto S. Tashiro; Toru Tamagawa; Shin Watanabe; Makio Yamaguchi; Kazutaka Yamaoka; Daisuke Yonetoku
  PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN, Volume：60, First page：S25, Last page：S33, Feb. 2008
  The hard X-ray detector (HXD) aboard the X-ray satellite Suzaku is designed to have a good timing capability with a 61 its time resolution. In addition to detailed descriptions of the HXD timing system, results of in-orbit timing calibration and the performance of the HXD are summarized. The relative accuracy of time measurements of the HXD event was confirmed to have an accuracy of 1.9 x 10(-9) s s(-1) per day, and the absolute timing was confirmed to be accurate to 360 mu s or better. The results were achieved mainly through observations of the Crab pulsar, including simultaneous ones with RXTE, INTEGRAL, and Swift.
  OXFORD UNIV PRESS, English
  DOI：https://doi.org/10.1093/pasj/60.sp1.S25
  DOI ID：10.1093/pasj/60.sp1.S25, ISSN：0004-6264, eISSN：2053-051X, Web of Science ID：WOS:000255818700003
• Testing the external-shock model of gamma-ray bursts using the late-time simultaneous optical and X-ray afterglows　　　　　　　　　　　　　　　
  Yuji Urata; Ryo Yamazaki; Takanori Sakamoto; Kuiyun Huang; Weikang Zheng; Goro Sato; Tsutomu Aoki; Jinsong Deng; Kunihito Ioka; WingHuen Ip; Koji S. Kawabata; YiHsi Lee; Liping Xin; Hiroyuki Mito; Takashi Miyata; Yoshikazu Nakada; Takashi Ohsugi; Yulei Qiu; Takao Soyano; Kenichi Tarusawa; Makoto Tashiro; Makoto Uemura; Jianyan Wei; Takuya Yamashita
  ASTROPHYSICAL JOURNAL, Volume：668, Number：2, First page：L95, Last page：L98, Oct. 2007
  We study the "normal" decay phase of the X- ray afterglows of gamma- ray bursts ( GRBs), which follows the shallow decay phase, using the events simultaneously observed in the R band. The classical external- shock model - in which neither the delayed energy injection nor time dependency of shock microphysics is considered shows that the decay indices of the X- ray and R- band light curves, alpha(x) and alpha(o), obey a certain relation, and that in particular, alpha(o) - alpha(x) should be larger than -1/4 unless the ambient density increases with the distance from the central engine. For our selected 14 samples, we have found that four events violate the limit at more than the 3 sigma level, so that a fraction of events are outliers of the classical external-shock model at the "normal" decay phase.
  IOP PUBLISHING LTD, English
  DOI：https://doi.org/10.1086/522930
  DOI ID：10.1086/522930, ISSN：0004-637X, eISSN：1538-4357, Web of Science ID：WOS:000250083000001
• 「すざく」衛星による2006年12月5日のX9.0太陽フレアからの中性子検出の可能性　　　　　　　　　　　　　　　
  北口貴雄; 榎戸輝揚; 中澤知洋; 牧島一夫; 国分紀秀; 川原田円; 寺田幸功; 遠藤輝; 浦田裕次; 田代信; 山岡和貴; HONG S; 土屋晴文; LOWENSTEIN Michael
  日本物理学会講演概要集, Volume：62, Number：2, First page：103, Last page：103, 21 Aug. 2007
  The Physical Society of Japan (JPS), Japanese
  ISSN：1342-8349, J-Global ID：200902206070066105, CiNii Articles ID：110007193860, CiNii Books ID：AA11439205
• 「すざく」衛星硬X線検出器(HXD)主検出部の現状(IV)　　　　　　　　　　　　　　　
  国分紀秀; 高橋忠幸; 渡辺伸; 中澤知洋; 牧島一夫; 寺田幸功; 川原田円; 玉川徹; 深沢泰司; 水野恒史; 高橋弘充; 田代信; 山岡和貴; 村上敏夫; 米徳大輔
  日本物理学会講演概要集, Volume：62, Number：2, First page：105, Last page：105, 21 Aug. 2007
  The Physical Society of Japan (JPS), Japanese
  ISSN：1342-8349, J-Global ID：200902289252680545, CiNii Articles ID：110007194127, CiNii Books ID：AA11439205
• Initial Results from the Suzaku Wide-band All-sky Monitor　　　　　　　　　　　　　　　
  YAMAOKA Kazutaka; OHNO Masanori; TASHIRO Makoto; 「Suzaku」WAM Team
  The Astronomical herald, Volume：100, Number：9, First page：452, Last page：461, 20 Aug. 2007
  Japanese
  ISSN：0374-2466, CiNii Articles ID：10024590052, CiNii Books ID：AN00154555
• A multiband study of the optically dark GRB 051028　　　　　　　　　　　　　　　
  Yuji Urata; Kui-Yun Huang; Ping-Hung Kuo; Wing-Huen Ip; Yulei Qiu; Keisuke Masuno; Makoto Tashiro; Keiichi Abe; Kaori Onda; Natsuki Kodaka; Makoto Kuwahara; Toru Tamagawa; Fumihiko Usui; Kunihito Ioka; Yi-Hsi Lee; Jianyan Wei; Jinsong Deng; Weikang Zheng; Kazuo Makishimai
  PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN, Volume：59, Number：4, First page：L29, Last page：L33, Aug. 2007
  Observations were made of the optical afterglow of GRB 051028 with the Lulin observatory 1.0 m telescope and the Wide-Field Telescope for GRB Early Timing (WIDGET) robotic telescope system. R-band photometric data were obtained on 2005 October 28 (UT), or 0.095-0.180 d after the burst. There is a possible plateau in the optical light curve around 0.1 d after the burst; the afterglow of GRB 051028 resembles optically bright afterglows (e.g., GRB 041006, GRB 050319, GRB 060605) in shape of the light curve, but not in brightness. The brightness of the GRB 051028 afterglow is 3 mag fainter than that of one of the dark events, GRB 020124. Optically dark GRBs have been attributed to dust extinction within the host galaxy or a high redshift. However, a spectrum analysis of the X-rays implies that there is no significant absorption by the host galaxy. Furthermore, according to a theoretical calculation of the Ly alpha absorption to find the limit of the GRB 051028's redshift, the expected R-band absorption is not high enough to explain the darkness of the afterglow. The present results disfavor either the high-redshift hypothesis or the high-extinction scenario for optically dark bursts; rather, they are consistent with the possibility that the brightness of the optical afterglow is intrinsically dark.
  OXFORD UNIV PRESS, English, Report scientific journal
  DOI：https://doi.org/10.1093/pasj/59.4.L29
  DOI ID：10.1093/pasj/59.4.L29, ISSN：0004-6264, eISSN：2053-051X, Web of Science ID：WOS:000249977200003
• Probing the disk-jet connection of the radio galaxy 3C 120 observed with Suzaku　　　　　　　　　　　　　　　
  Jun Kataoka; James N. Reeves; Kazushi Iwasawa; Alex G. Markowitz; Richard F. Mushotzky; Makoto Arimoto; Tadayuki Takahashi; Yoshihiro Tsubuku; Masayoshi Ushio; Shin Watanabe; Luigi C. Gallo; Greg M. Madejski; Yuichi Terashima; Naoki Isobe; Makoto S. Tashiro; Takayoshi Kohmura
  PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN, Volume：59, Number：2, First page：279, Last page：297, Apr. 2007
  We report on deep (40 ks x 4) observations of the bright broad line radio galaxy 3C 120 using Suzaku. The observations were spaced one week apart, and sampled a range of continuum fluxes. An excellent broadband spectrum was obtained over two decades of frequency (0.6 to 50 keV) within each 40 ks exposure. We clearly resolved the iron K emission-line complex, finding that it consists of a narrow K alpha core (sigma similar or equal to 110 eV or an EW of 60 eV), a 6.9 keV line, and an underlying broad iron line. Our confirmation of the broad line contrasts with the XMM-Newton observation in 2003, where the broad line was not required. The most natural interpretation of the broadline is iron Kline emission from a face-on accretion disk that is truncated at similar to 10 r(g). Above 10 keV, a relatively weak Compton hump was detected (reflection fraction of R similar or equal to 0.6), superposed on the primary X-ray continuum of Gamma similar or equal to 1.75. Thanks to the good photon statistics and low background of the Suzaku data, we clearly confirm the spectral evolution of 3C 120, whereby the variability amplitude decreases with increasing energy. More strikingly, we discovered that the variability is caused by a steep power-law component of Gamma similar or equal to 2.7, possibly related to non-thermal jet emission. We discuss our findings in the context of similarities and differences between radio-loud/quiet objects.
  OXFORD UNIV PRESS, English
  DOI：https://doi.org/10.1093/pasj/59.2.279
  DOI ID：10.1093/pasj/59.2.279, ISSN：0004-6264, eISSN：2053-051X, Web of Science ID：WOS:000246404000003
• Swift discovery of gamma-ray bursts without a jet break feature in their X-ray afterglows　　　　　　　　　　　　　　　
  G. Sato; R. Yamazaki; K. Ioka; T. Sakamoto; T. Takahashi; K. Nakazawa; T. Nakamura; K. Toma; D. Hullinger; M. Tashiro; A. M. Parsons; H. A. Krimm; S. D. Barthelmy; N. Gehrels; D. N. Burrows; P. T. O'Brien; J. P. Osborne; G. Chincarini; D. Q. Lamb
  ASTROPHYSICAL JOURNAL, Volume：657, Number：1, First page：359, Last page：366, Mar. 2007
  We analyze Swift gamma-ray bursts (GRBs) and X-ray afterglows for three GRBs with spectroscopic redshift determinations: GRB 050401, XRF 050416a, and GRB 050525a. We find that the relation between spectral peak energy and isotropic energy of prompt emissions (the Amati relation) is consistent with that for the bursts observed in the pre-Swift era. However, we find that the X-ray afterglow light curves, which extend up to 10-70 days, show no sign of the jet break that is expected in the standard framework of collimated outflows. We do so by showing that none of the X-ray afterglow light curves in our sample satisfy the relation between the spectral and temporal indices that is predicted for the phase after jet break. The jet break time can be predicted by inverting the tight empirical relation between the peak energy of the spectrum and the collimation-corrected energy of the prompt emission (the Ghirlanda relation). We find that there are no temporal breaks within the predicted time intervals in X-ray band. This requires either that the Ghirlanda relation has a larger scatter than previously thought, that the temporal break in X-rays is masked by some additional source of X-ray emission, or that it does not happen for some unknown reason.
  IOP PUBLISHING LTD, English
  DOI：https://doi.org/10.1086/510610
  DOI ID：10.1086/510610, ISSN：0004-637X, eISSN：1538-4357, Web of Science ID：WOS:000244635300030
• 26aSF-6 X線観測衛星「すざく」搭載広帯域全天モニター(WAM)を用いた太陽フレアの観測と性能評価(26aSF X線・γ線,宇宙線・宇宙物理領域)　　　　　　　　　　　　　　　
  鈴木 正信; 佐藤 優美; 浦田 裕次; 田代 信; 寺田 幸功; 山岡 和貴; 簑島 敬; 横山 央明; 牧島 一夫; 高橋 忠幸; HXD-WAMチーム
  Volume：62, Number：1, First page：95, Last page：95, 28 Feb. 2007
  Japanese
  ISSN：1342-8349, CiNii Articles ID：110007140777, CiNii Books ID：AA11439205
• 26aSF-8 Multiwavelength and simultaneous observation of TeV blazers with SUZAKU/H.E.S.S/MAGIC　　　　　　　　　　　　　　　
  Ushio Masayoshi; Aharonian F.; Costamante L.; Wagner S.
  Meeting abstracts of the Physical Society of Japan, Volume：62, Number：1, First page：95, Last page：95, 28 Feb. 2007
  The Physical Society of Japan (JPS), Japanese
  ISSN：1342-8349, CiNii Articles ID：110007140775, CiNii Books ID：AA11439205
• 27aSF-3 ガンマ線バースト閃光観測のための超広視野可視光カメラ(WIDGET)の改良と性能評価(27aSF X線・γ線,宇宙線・宇宙物理領域)　　　　　　　　　　　　　　　
  小高 夏来; くわ原 允; 増野 圭輔; 玉川 徹; 浦田 裕次; 田代 信; 阿部 圭一; 恩田 香織; 臼井 文彦; 寺田 幸功; 征矢野 隆夫; 宮田 隆志; 中田 好一; 柳沢 賢一; WIDGETチーム
  Volume：62, Number：1, First page：103, Last page：103, 28 Feb. 2007
  Japanese
  ISSN：1342-8349, CiNii Articles ID：110007139236, CiNii Books ID：AA11439205
• Extensive multiband study of the X-ray rich GRB 050408 - A likely off-axis event with an intense energy injection　　　　　　　　　　　　　　　
  A. de Ugarte Postigo; T. A. Fatkhullin; G. Johannesson; J. Gorosabel; V. V. Sokolov; A. J. Castro-Tirado; Yu. Yu. Balega; O. I. Spiridonova; M. Jelinek; S. Guziy; D. Perez-Ramirez; J. Hjorth; P. Laursen; D. Bersier; S. B. Pandey; M. Bremer; A. Monfardini; K. Y. Huang; Y. Urata; W. H. Ip; T. Tamagawa; D. Kinoshita; T. Mizuno; Y. Arai; H. Yamagishi; T. Soyano; F. Usui; M. Tashiro; K. Abe; K. Onda; Z. Aslan; I. Khamitov; T. Ozisik; U. Kiziloglu; I. Bikmaev; N. Sakhibullin; R. Burenin; M. Pavlinsky; R. Sunyaev; D. Bhattacharya; A. P. Kamble; C. H. Ishwara Chandra; S. A. Trushkin
  ASTRONOMY & ASTROPHYSICS, Volume：462, Number：3, First page：L57, Last page：U9, Feb. 2007
  Aims. Understand the shape and implications of the multiband ligth curve of GRB050408, an X-ray rich (XRR) burst.
  Methods. We present a multiband optical light curve, covering the time from the onset of the.-ray event to several months after, when we only detect the host galaxy. Together with X-ray, millimetre and radio observations we compile what, to our knowledge, is the most complete multiband coverage of an XRR burst afterglow to date.
  Results. The optical and X-ray light curve is characterised by an early flattening and an intense bump peaking around 6 days after the burst onset. We explain the former by an off-axis viewed jet, in agreement with the predictions made for XRR by some models, and the latter with an energy injection equivalent in intensity to the initial shock. The analysis of the spectral flux distribution reveals an extinction compatible with a low chemical enrichment surrounding the burst. Together with the detection of an underlying starburst host galaxy we can strengthen the link between XRR and classical long-duration bursts.
  EDP SCIENCES S A, English
  DOI：https://doi.org/10.1051/0004-6361:20066660
  DOI ID：10.1051/0004-6361:20066660, ISSN：0004-6361, Web of Science ID：WOS:000243721900009
• 22aZJ-4 Current Status of the Suzaku Hard X-ray Detector Wide-band All-sky Monitor(III)　　　　　　　　　　　　　　　
  Hong S; Yamaoka K; Nakagawa Y.E; Sugita S; Kokubun M; Watanabe S; Suzuki M; Fukazawa Y; Mizuno T; Ohno M; Takahashi T; Tashiro M; Uehara T; Kira C; Nakazawa K; Enoto T; Yamauchi M; Sonoda E; Maeno S; Tanaka H; Hara R; Urata Y; Onda K; Suzuki M; Kodaka N; Morigami K; Terada Y; Tamagawa T
  Meeting Abstracts of the Physical Society of Japan, Volume：62, Number：0, First page：106, Last page：106, 2007
  The Physical Society of Japan, Japanese
  ISSN：1342-8349, CiNii Articles ID：110007194125, CiNii Books ID：AA11439205
• 26aSF-3 Current Status of the Suzaku Hard X-ray Detector (III)　　　　　　　　　　　　　　　
  Kokubun M; Fukazawa Y; Mizuno T; Takahashi H; Tashiro S; Yamaoka K; Murakami T; Yonetoku D; Suzaku HXD team; Takahashi T; Nakazawa K; Watanabe S; Kawaharada M; Makishima K; Terada Y; Tamagawa T; Kubota A
  Meeting Abstracts of the Physical Society of Japan, Volume：62, Number：0, First page：94, Last page：94, 2007
  一般社団法人 日本物理学会, Japanese
  ISSN：1342-8349, CiNii Articles ID：110007140780, CiNii Books ID：AA11439205
• Suzaku Study of hard X-ray Emission from Nearby Galaxy Clusters　　　　　　　　　　　　　　　
  OTA Naomi; Kitaguchi, T; Nakazawa, N; Makishima, K; Kawaharada, M; Ota, N; Kokubun, M; Yamasaki, N; Kawano, N; Fukazawa, Y; Sato, K; Ohashi, T; Murase, K; Urata, Y; Tashiro, M; Furusawa, A; Suzaku Team
  XMM-Newton: The Next Decade, 2007
• 「すざく」衛星ガンマ線バースト残光観測の顛末　　　　　　　　　　　　　　　
  田代 信
  Volume：100, First page：254, Last page：263, 2007
• The X-ray observatory Suzaku　　　　　　　　　　　　　　　
  Kazuhisa Mitsuda; Mark Bautz; Hajime Inoue; Richard L. Kelley; Katsuji Koyama; Hideyo Kunieda; Kazuo Makshima; Yoshiaki Ogawara; Robert Petre; Tadayuki Takahashi; Hiroshi Tsunemi; Nicholas E. White; Naohisa Anabuki; Lorella Angelini; Keith Arnaud; Hisamitsu Awaki; Aya Bamba; Kevin Boyce; Gregory V. Brown; Kai-Wing Chan; Jean Cottam; Tadayasu Dotanli; John Doty; Ken Ebisawa; Yuichiro Ezoe; Andrew C. Fabian; Enectali Figueroa; Ryuichi Fujimoto; Yasushi Fukazawa; Tae Furusho; Akihiro Furuzawa; Keith Gendreau; Richard E. Griffiths; Yoshito Haba; Kenji Hamaguchi; Ilana Harrus; Gunther Hasinger; Isamu Hatsukade; Kiyoshi Hayashida; Patrick J. Henry; Junko S. Hiraga; Stephen S. Holt; Ann Hornschemeier; John P. Hughes; Una Hwang; Manabu Ishida; Yoshitaka Ishisaki; Naoki Isobe; Masayuki Itoh; Naoko Iyomoto; Steven M. Kahn; Tuneyoshi Kamae; Hideaki Katagiri; Jun Kataoka; Haruyoshi Katayama; Nobuyuki Kawai; Caroline Kilbourne; Kenzo Kinugasa; Steve Kissel; Shunji Kitamoto; Mitsuhiro Kohama; Takayoshi Kohmura; Motohide Kokubun; Taro Kotani; Jun'ichi Kotoku; Aya Kubota; Greg M. Madejski; Yoshitomo Maeda; Fumiyoshi Makino; Alex Markowitz; Chiho Matsumoto; Hironori Matsumoto; Masaru Matsuoka; Kyoko Matsushita; Dan McCammon; Tatehiko Mihara; Kazutami Misaki; Emi Miyata; Tsunefumi Mizuno; Koji Mori; Hideyuki Mori; Mikio Morii; Harvey Moseley; Koji Mukai; Hiroshi Murakami; Toshio Murakami; Richard Mushotzky; Fumiaki Nagase; Masaaki Namiki; Hitoshi Negoro; Kazubiro Nakazawa; John A. Nousek; Takashi Okajima; Yasushi Ogasaka; Takaya Ohashi; Tai Oshima; Naomi Ota; Masanobu Ozaki; Hideki Ozawa; Arvind N. Parmar; William D. Pence; F. Scott Porter; James N. Reeves; George R. Ricker; Ikuya Sakurai; Wilton T. Sanders; Atsushi Senda; Peter Serlemitsos; Ryo Shibata; Yang Soong; Randall Smith; Motoko Suzuki; Andrew E. Szymkowiak; Hiromitsu Takahashi; Torn Tamagawa; Keisuke Tamura; Takayuki Tamura; Yasuo Tanaka; Makoto Tashiro; Yuzuru Tawara; Yukikatsu Terada; Yuichi Terashima; Hiroshi Tomida; Ken'ichi Torii; Yohko Tsuboi; Masahiro Tsujimoto; Takeshi Go Tsuru; Martin J. L. Turner; Yoshihiro Ueda; Shiro Ueno; Masaru Ueno; Shin'ichiro Uno; Yuji Urata; Shin Watanabe; Norimasa Yamamoto; Kazutaka Yamaoka; Noriko Y. Yamasaki; Koujun Yamashita; Makoto Yamauchi; Shigeo Yamauchi; Tahir Yaqoob; Daisuke Yonetoku; Atsumasa Yoshida
  PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN, Volume：59, First page：S1, Last page：S7, Jan. 2007
  High-sensitivity wide-band X-ray spectroscopy is the key feature of the Suzaku X-ray observatory, launched on 2005 July 10. This paper summarizes the spacecraft, in-orbit performance, operations, and data processing that are related to observations. The scientific instruments, the high-throughput X-ray telescopes, X-ray CCD cameras, non-imaging hard X-ray detector are also described.
  OXFORD UNIV PRESS, English
  DOI：https://doi.org/10.1093/pasj/59.sp1.S1
  DOI ID：10.1093/pasj/59.sp1.S1, ISSN：0004-6264, eISSN：2053-051X, Web of Science ID：WOS:000244441700001
• Swift and Suzaku observations of the X-ray afterglow from the GRB 060105　　　　　　　　　　　　　　　
  Makoto S. Tashiro; Keiichi Abe; Lorella Angelini; Scott Barthelmy; Neil Gehrels; Nobuyuki Ishikawa; Louis J. Kaluzienski; Nobuyuki Kawai; Richard L. Kelley; Kenzo Kinugasa; Hironobu Kodaira; Takayoshi Kohmura; Kaori Kubota; Yoshitomo Maeda; Shouta Maeno; Hiroshi Murakami; Toshio Murakami; Yujin E. Nakagawa; Kazuhiro Nakazawa; John Nousek; Shin'ya Okuno; Kaori Onda; James N. Reeves; George Ricker; Goro Sato; Eri Sonoda; Motoko Suzuki; Tadayuki Takahashi; Toru Tamagawa; Ken'ichi Torii; Yoshihiro Ueda; Yuji Urata; Kazutaka Yamaoka; Makoto Yamauchi; Daisuke Yonetoku; Atsumasa Yoshida; Satoru Yoshinari
  PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN, Volume：59, First page：S361, Last page：S367, Jan. 2007
  Results are presented of early X-ray afterglow observations of GRB 060105 by Swift and Suzaku. The bright, long gamma-ray burst GRB; 060105 triggered the Swift Burst Alert Telescope at 06:49:28 on 2006 January 5 (T-0). The Suzaku team commenced a pre-planned target of opportunity observation at 19 ks (5.3 hr) after the Swift trigger. The X-ray flux faded during observations from 6.8 x 10(-9) ergs(-1) cm(-2) (at T-0 + 87 s with the Swift/XRT) to 1.5 x 10(-13) erg s(-1) cm(-2) [at T-0 + 94-101 ks with the Suzaku X-ray Imaging Spectrometer (XIS)] in the 2-10 keV energy band. Following prompt emission and successive very steep decay, a shallow decay was observed from To + 187 s to T-0 + 1287 s. After an observation gap during T-0 + (1.5-3) ks, an extremely early steep decay was observed in T-0 + (4-30) ks. The lightcurve flattened again at T-0 + 30ks, and another steep decay followed from T-0 + 50ks to the end of observations. Both steep decays exhibited decay indices of 2.3-2.4. This very early break, if it is a jet break, is the earliest case among X-ray afterglow observations, suggesting a very narrow jet whose opening angle is well below 1 degrees. The unique Suzaku/XIS data allow us to set very tight upper limits on line emission or absorption in this GRB. For the reported pseudo-redshift of z = 4.0 +/- 1.3 the upper limit on the iron line equivalent width is 50 eV.
  OXFORD UNIV PRESS, English
  DOI：https://doi.org/10.1093/pasj/59.sp1.S361
  DOI ID：10.1093/pasj/59.sp1.S361, ISSN：0004-6264, eISSN：2053-051X, Web of Science ID：WOS:000244441700030
• Multicolor shallow decay and chromatic breaks in the GRB 050319 optical afterglow　　　　　　　　　　　　　　　
  K. Y. Huang; Y. Urata; P. H. Kuo; W. H. Ip; K. Ioka; T. Aoki; C. W. Chen; W. P. Chen; M. Isogai; H. C. Lin; K. Makishima; H. Mito; T. Miyata; Y. Nakada; S. Nishiura; K. Onda; Y. Qiu; T. Soyano; T. Tamagawa; K. Tarusawa; M. Tashiro; T. Yoshioka
  ASTROPHYSICAL JOURNAL, Volume：654, Number：1, First page：L25, Last page：L28, Jan. 2007
  Multiwavelength observations of the optical afterglow of GRB 050319 were performed from 1.31 to 9.92 hr after the burst. Our R-band light curves, combined with other published data, can be described by the smooth broken power-law function, with alpha(1) = -0.84 +/- 0.02 to alpha(2) = -0.48 +/- 0.03, 0.04 days after the gamma-ray burst. The optical light curves are characterized by shallow decays - as was also observed in the X-rays - which may have a similar origin, related to energy injection. However, our observations indicate that there is still a puzzle concerning the chromatic breaks in the R-band light curve (at 0.04 days) and the X-ray light curve (at 0.004 days) that remains to be solved.
  IOP PUBLISHING LTD, English
  DOI：https://doi.org/10.1086/510737
  DOI ID：10.1086/510737, ISSN：0004-637X, eISSN：1538-4357, Web of Science ID：WOS:000243222200007
• In-orbit performance of the hard X-ray Detector on board Suzaku　　　　　　　　　　　　　　　
  Motohide Kokubun; Kazuo Makishima; Tadayuki Takahashi; Toshio Murakami; Makoto Tashiro; Yasushi Fukazawa; Tuneyoshi Kamae; Greg M. Madejski; Kazuhiro Nakazawa; Kazutaka Yamaoka; Yukikatsu Terada; Daisuke Yonetoku; Shin Watanabe; Toru Tamagawa; Tsunefumi Mizuno; Aya Kubota; Naoki Isobe; Isao Takahashi; Goro Sato; Hiromitsu Takahashi; Soojing Hong; Madoka Kawaharada; Naomi Kawano; Takefumi Mitani; Mio Murashima; Masaya Suzuki; Keiichi Abe; Ryouhei Miyawaki; Masanori Ohno; Takaaki Tanaka; Takayuki Yanagida; Takeshi Itoh; Kousuke Ohnuki; Ken-ichi Tamura; Yasuhiko Endo; Shinya Hirakuri; Tatsuro Hiruta; Takao Kitaguchi; Tetsuichi Kishishita; Satoshi Sugita; Takuya Takahashi; Shin'ichiro Takeda; Teruaki Enoto; Ayumi Hirasawa; Jun'ichiro Katsuta; Satoshi Matsumura; Kaori Onda; Mitsuhiro Sato; Masayoshi Ushio; Shin-nosuke Ishikawa; Koichi Murase; Hirokazu Odaka; Masanobu Suzuki; Yuichi Yaji; Shinya Yamada; Tomonori Yamasaki; Takayuki Yuasa
  PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN, Volume：59, First page：S53, Last page：S76, Jan. 2007
  The in-orbit performance and calibration of the Hard X-ray Detector (HXD) on board the X-ray astronomy satellite Suzaku are described. Its basic performances, including a wide energy bandpass of 10-600keV, energy resolutions of similar to 4 keV (FWHM) at 40 keV and similar to 11% at 511 keV, and a high background rejection efficiency, have been confirmed by extensive in-orbit calibrations. The long-term gains of PIN-Si diodes have been stable within 1% for half a year, and those of scintillators have decreased by 5-20%. The residual non-X-ray background of the HXD is the lowest among past non-imaging hard X-ray instruments in energy ranges of 15-70 and 150-500 keV. We provide accurate calibrations of energy responses, angular responses, timing accuracy of the HXD, and relative normalizations to the X-ray CCD cameras using multiple observations of the Crab Nebula.
  OXFORD UNIV PRESS, English
  DOI：https://doi.org/10.1093/pasj/59.sp1.S53
  DOI ID：10.1093/pasj/59.sp1.S53, ISSN：0004-6264, eISSN：2053-051X, Web of Science ID：WOS:000244441700005
• Hard X-ray Detector (HXD) on board Suzaku　　　　　　　　　　　　　　　
  Tadayuki Takahashi; Keiichi Abe; Manabu Endo; Yasuhiko Endo; Yuuichiro Ezoe; Yasushi Fukazawa; Masahito Hamaya; Shinya Hirakuri; Soojing Hong; Michihiro Horii; Hokuto Inoue; Naoki Isobe; Takeshi Itoh; Naoko Iyomoto; Tuneyoshi Kamae; Daisuke Kasama; Jun Kataoka; Hiroshi Kato; Madoka Kawaharada; Naomi Kawano; Kengo Kawashima; Satoshi Kawasoe; Tetsuichi Kishishita; Takao Kitaguch; Yoshihito Kobayashi; Motohide Kokubun; Jun'ichi Kotoku; Manabu Kouda; Aya Kubota; Yoshikatsu Kuroda; Greg Madejski; Kazuo Makishima; Kazunori Masukama; Yukari Matsumoto; Takefumi Mitani; Ryohei Miyawaki; Tsunefumi Mizuno; Kunishiro Mori; Masanori Mori; Mio Murashima; Toshio Murakami; Kazuhiro Nakazawa; Hisako Niko; Masaharu Nomachi; Yuu Okada; Masanori Ohno; Kousuke Oonuki; Naomi Ota; Hideki Ozawa; Goro Sato; Shingo Shinoda; Masahiko Sugiho; Masaya Suzuki; Koji Taguchi; Hiromitsu Takahashi; Isao Takahashi; Shin'ichiro Takeda; Ken-ichi Tamura; Takayuki Tamura; Takaaki Tanaka; Chiharu Tanihata; Makoto Tashiro; Yukikatsu Terada; Shin'ya Tominaga; Yasunobu Uchiyama; Shin Watanabe; Kazutaka Yamaoka; Takayuki Yanagida; Daisuke Yonetoku
  PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN, Volume：59, First page：S35, Last page：S51, Jan. 2007
  The Hard X-ray Detector (HXD) on board Suzaku covers a wide energy range from 10 keV to 600 keV by the combination of silicon PIN diodes and GSO scintillators. The HXD is designed to achieve an extremely low in-orbit background based on a combination of new techniques, including the concept of a well-type active shield counter. With an effective area of 142 cm(2) at 20 keV and 273 cm(2) at 150 keV, the background level at sea level reached similar to 1 X 10(-5) cts s(-1) cm(-2) keV(-1) at 30 keV for the PIN diodes, and similar to 2 X 10(-5) cts s(-1) cm(-2) keV(-1) at 100 keV, and similar to 7 X 10(-6) cts s(-1) cm(-2) keV(-1) at 200 keV for the phoswich counter. Tight active shielding of the HXD results in a large array of guard counters surrounding the main detector parts. These anti-coincidence counters, made of similar to 4 cm thick BGO crystals, have a large effective area for sub-MeV to MeV gamma-rays. They work as an excellent gamma-ray burst monitor with limited angular resolution (similar to 5 degrees). The on-board signal-processing system and the data transmitted to the ground are also described.
  OXFORD UNIV PRESS, English
  DOI：https://doi.org/10.1093/pasj/59.sp1.S35
  DOI ID：10.1093/pasj/59.sp1.S35, ISSN：0004-6264, eISSN：2053-051X, Web of Science ID：WOS:000244441700004
• 「すざく」衛星ガンマ線バースト残光観測の顛末　　　　　　　　　　　　　　　
  田代 信
  天文月報, Volume：100, First page：254, Last page：263, 2007
• Capability and strategy of the X-ray afterglow observation with Suzaku　　　　　　　　　　　　　　　
  M. S. Tashiro; T. Murakami; A. Yoshida; N. Kawai; J. Nousek; L. Angelini; J. L. Kaluzienski; L. R. Kelley; K. Kinugasa; K. Nakazawa; N. J. Reeves; G. Ricker; M. Suzuki; T. Takahashi; T. Tamagawa; K. Torii; Y. Ueda; Y. Urata; K. Yamaoka; M. Yamauchi; D. Yonetoku
  NUOVO CIMENTO DELLA SOCIETA ITALIANA DI FISICA B-BASIC TOPICS IN PHYSICS, Volume：121, Number：12, First page：1597, Last page：1598, Dec. 2006
  The Japanese X-ray astronomical satellite Suzaku launched in July 2005 is equipped with two kinds of X-ray instruments for the wide-band spectroscopy. The X-ray CCD cameras (XIS) cover 0.3 to 12 keV with the energy resolution of 120eV at 6keV. The Hard X-ray Detector (HXD) consisting of well-type phoswitch counters covers 40-600keV. With these instruments, we organized a team for quick follow-up observations of gamma-ray bursts, aiming to observe the afterglow phase transition and to search for spectral features with the wide band X-ray instruments.
  SOC ITALIANA FISICA, English
  DOI：https://doi.org/10.1393/neb/i2007-10323-9
  DOI ID：10.1393/neb/i2007-10323-9, ISSN：2037-4895, eISSN：1594-9982, Web of Science ID：WOS:000250546900066
• When do internal shocks end and external shocks begin? Early-time broadband modeling of GRB 051111　　　　　　　　　　　　　　　
  N. R. Butler; W. Li; D. Perley; K. Y. Huang; Y. Urata; J. X. Prochaska; J. S. Bloom; A. V. Filippenko; R. J. Foley; D. Kocevski; H. -W. Chen; Y. Qiu; P. H. Kuo; F. Y. Huang; W. H. Ip; T. Tamagawa; K. Onda; M. Tashiro; K. Makishima; S. Nishihara; Y. Sarugaku
  ASTROPHYSICAL JOURNAL, Volume：652, Number：2, First page：1390, Last page：1399, Dec. 2006
  Even with the renaissance in gamma-ray burst (GRB) research fostered by the Swift satellite, few bursts have both contemporaneous observations at long wavelengths and exquisite observations at later times across the electromagnetic spectrum. We present here contemporaneous imaging with the KAIT robotic optical telescope, dense optical sampling with Lulin, supplemented with infrared data from PAIRITEL and radio to gamma-ray data from the literature. For the first time, we can test the constancy of microphysical parameters in the internal-external shock paradigm and carefully trace the flow of energy from the GRB to the surrounding medium. KAIT data taken P1 minute after the start of GRB 051111 and coinciding with the fading gamma-ray tail of the prompt emission indicate a smooth reinjection of energy into the shock. No color change is apparent in observations beginning similar to 1.5 minutes after the GRB and lasting for the first hour after the burst. There are achromatic flux modulations about the best-fit model at late (t approximate to 10(4) s) times, possibly due to variations in the external density. We find that the host galaxy extinction is well fit by a curve similar to that of the Small Magellanic Cloud. Low visual extinction, A(V) approximate to 0.2 mag, combined with high column densities determined from the X-ray and optical spectroscopy (N-H > 10(21) cm(-2)), indicate a low dust-to-metals ratio and a possible overabundance of the light metals. An apparent small ratio of total to selective extinction (R-V approximate to 2) argues against dust destruction by the GRB. Time constancy of both the IR/optical/UV spectral energy distribution and the soft X-ray absorption suggests that the absorbing material is not local to the GRB.
  IOP PUBLISHING LTD, English, Book review
  DOI：https://doi.org/10.1086/508624
  DOI ID：10.1086/508624, ISSN：0004-637X, eISSN：1538-4357, Web of Science ID：WOS:000242530100049
• 「すざく」衛星による銀河団からの非熱的硬X線放射の探査
  川埜直美; 深澤泰司; 北口貴雄; 川原田円; 国分紀秀; 牧島一夫; 中澤知洋; 山崎典子; 太田直美; 佐藤浩介; 大橋隆哉; 村瀬弘一; 浦田裕次; 田代信
  日本天文学会年会講演予稿集, Volume：2006, First page：193, 20 Aug. 2006
  Japanese
  ISSN：1347-0639, J-Global ID：201302244530353134
• Swift衛星と「すざく」衛星によるGRB060105の早期X線残光の観測
  田代信; 浦田裕次; 阿部圭一; 恩田香織; 村上敏夫; 米徳大輔; 奥野晋也; 小平裕宣; 吉成覚; 吉田篤正; 山岡和貴; 中川友進; 石川信行; 山内誠; 園田絵里; 前野将太; 高橋忠幸; 中澤知洋; 村上弘志; 玉川徹; 鈴木素子; 河合誠之; NOUSEK J; 上田佳宏; 久保田香織; 鳥居研一; 衣笠健三; 幸村孝由; KELLY R; ANGELINI L; REEVES J; KALUZIENSKI L; GEHRELS N; BARTHELMY S; 佐藤悟朗; RICKER G
  日本天文学会年会講演予稿集, Volume：2006, First page：70, 20 Aug. 2006
  Japanese
  ISSN：1347-0639, J-Global ID：201302279462097777
• 「すざく」衛星搭載硬X線検出器(HXD)主検出部の現状(II)
  国分紀秀; 川原田円; 牧島一夫; 寺田幸功; 山岡和貴; 高橋忠幸; 中澤知洋; 渡辺伸; 深沢泰司; 水野恒史; 高橋弘充; 田代信; 米徳大輔; 村上敏夫
  日本天文学会年会講演予稿集, Volume：2006, First page：264, 20 Aug. 2006
  Japanese
  ISSN：1347-0639, J-Global ID：201302286233674929
• 「すざく」搭載硬X線検出器GSOシンチレータのゲイン履歴補正およびバックグラウンドモデル化の現状
  山崎智紀; 平澤歩; 高橋弘充; 深沢泰司; 山田真也; 伊藤健; 北口貴雄; 国分紀秀; 牧島一夫; 鈴木正信; 田代信; 磯部直樹; 寺田幸功; 中澤知洋; 高橋忠幸
  日本天文学会年会講演予稿集, Volume：2006, First page：265, 20 Aug. 2006
  Japanese
  ISSN：1347-0639, J-Global ID：201302289337226889
• 23pSH-5 A search for hard X-ray emission from galaxy clusters using Suzaku　　　　　　　　　　　　　　　
  Kitaguchi T; Kawaharada M; Kokubun M; Makishima K; ota N; Fukazawa Y; Kawano N; Nakazawa K; Yamasaki N; Sato K; Ohashi T; Murase K; Urata Y; Tashiro M; Suzaku team
  Meeting abstracts of the Physical Society of Japan, Volume：61, Number：2, First page：77, Last page：77, 18 Aug. 2006
  The Physical Society of Japan (JPS), Japanese
  ISSN：1342-8349, CiNii Articles ID：110007183663, CiNii Books ID：AA11439205
• The XMM-Newton examination of energetics in the east lobe of the nearby radio galaxy Fornax A (NGC 1316)　　　　　　　　　　　　　　　
  N. Isobe; K. Makishima; M. Tashiro; K. Itoh; N. Iyomoto; I. Takahashi; H. Kaneda
  ASTROPHYSICAL JOURNAL, Volume：645, Number：1, First page：256, Last page：263, Jul. 2006
  An XMM-Newton observation of the east radio lobe of the nearby radio galaxy Fornax A is reported. The diffuse hard X-ray emission associated with the east lobe, which was initially discovered by ASCA and ROSAT, is confirmed with significant signal statistics, after strictly removing 59 sources detected within the MOS field of view. Its X-ray spectrum is described by a single power-law model, which is absorbed by a medium with a column density consistent with that toward the object. The best-fit X-ray photon index, Gamma(X) = 1.62(-0.15)(+0.24), agrees with the synchrotron radio index, Gamma(R) = 1.68 +/- 0.1, determined from the radio spectrum between 29.9 MHz and 5 GHz. Hence, the inverse Compton interpretation for the diffuse X-rays is justified. The X-ray flux density in the east lobe is measured to be 90 +/- 21 nJy at 1 keV (including both statistical and systematic errors) with the index fixed at the radio value. This gives electron and magnetic energy densities of 3.0(-1.0)(+1.5) x 10(-13) and 6.1(-3.5)(+5.7) x 10(-14) ergs cm(-3), respectively. The latter corresponds to a magnetic field strength of 1.24(-0.40)(+0.50) mu G, which is smaller than the field estimated under the minimum energy condition, 1.55 mu G, although with a slightly large error. Reevaluation is also made of the ASCA result on the west lobe, to show that both lobes share a similar physical condition in terms of energetics.
  UNIV CHICAGO PRESS, English
  DOI：https://doi.org/10.1086/504253
  DOI ID：10.1086/504253, ISSN：0004-637X, Web of Science ID：WOS:000238832900019
• X線天文衛星「すざく」による観測速報(3)　　　　　　　　　　　　　　　
  田代 信; 山岡 和貴; 大野 雅功; 村上 敏夫; 中澤 知洋; 中川 友進; 河合 誠之; 高橋 忠幸; 寺田 幸功
  Volume：99, Number：5, First page：282, Last page：283, 20 Apr. 2006
  Japanese
  ISSN：0374-2466, CiNii Articles ID：10018138467, CiNii Books ID：AN00154555
• 28aTF-1 In-Orbit Calibration of the HXD-II onboard Suzaku　　　　　　　　　　　　　　　
  Kitaguchi T.; Kokubun M.; Hirakuri S.; Miyawaki R.; Makishima K.; Terada Y.; Kishishita T.; Nakazawa K.; Takahashi T.; Endo Y.; Tashiro M.; Fukazawa Y.; the HXD team
  Meeting abstracts of the Physical Society of Japan, Volume：61, Number：1, First page：92, Last page：92, 04 Mar. 2006
  The Physical Society of Japan (JPS), Japanese
  ISSN：1342-8349, CiNii Articles ID：110007179582, CiNii Books ID：AA11439205
• 28pTF-14 超広視野可視光カメラ(WIDGET)の改良とガンマ線バースト観測結果(28pTF X線・γ線,宇宙線・宇宙物理領域)　　　　　　　　　　　　　　　
  桑原 允; 吾妻 洋樹; 玉川 徹; 浦田 裕次; 寺田 幸功; 田代 信; 阿部 圭一; 恩田 香織; 臼井 文彦; WIDGETチーム
  Volume：61, Number：1, First page：99, Last page：99, 04 Mar. 2006
  Japanese
  ISSN：1342-8349, CiNii Articles ID：110007177186, CiNii Books ID：AA11439205
• 「すざく」ファーストライト:硬X線検出器(HXD‐II)
  国分紀秀; 高橋弘充; 牧島一夫; 山岡和貴; 高橋忠幸; 中澤知洋; 渡辺伸; 深沢泰司; 水野恒史; 寺田幸功; 田代信; 米徳大輔; 村上敏夫; 能町正治; 釜江常好; MADEJSKI Greg
  日本天文学会年会講演予稿集, Volume：2006, First page：280, 20 Feb. 2006
  Japanese
  ISSN：1347-0639, J-Global ID：201302217149968532
• すざく衛星搭載PIN型シリコン検出器の軌道上較正及び性能評価
  岸下徹一; 高橋忠幸; 中澤知洋; 渡辺伸; 田中孝明; 田村健一; 牧島一夫; 国分紀秀; 宮脇良平; 北口貴雄; 平栗慎也; 寺田幸功; 田代信; 遠藤康彦; 深沢泰司; 川埜直美; 平澤歩
  日本天文学会年会講演予稿集, Volume：2006, First page：249, 20 Feb. 2006
  Japanese
  ISSN：1347-0639, J-Global ID：201302223073460950
• 「すざく」衛星搭載の硬X線検出器HXD主検出部の現状
  中澤知洋; 釜江常好; 久保田あや; 国分紀秀; 高橋忠幸; 高橋弘充; 田代信; 玉川徹; 寺田幸功; 能町正治; 深沢泰司; 牧島一夫; 水野恒史; 村上敏夫; 山岡和貴; 米徳大輔; 渡辺伸; MADEJSKI Greg
  日本天文学会年会講演予稿集, Volume：2006, First page：248, 20 Feb. 2006
  Japanese
  ISSN：1347-0639, J-Global ID：201302257447818626
• 「すざく」広帯域全天モニタ(WAM)のバックグラウンド解析
  高橋拓也; 大野雅功; 深沢泰司; 杉田聡司; 山岡和貴; 遠藤康彦; 田代信; 榎戸輝揚; 宮脇良平; 国分紀秀; 佐藤悟朗; 中澤知洋; 高橋忠幸; 寺田幸功; 玉川徹; 牧島一夫
  日本天文学会年会講演予稿集, Volume：2006, First page：250, 20 Feb. 2006
  Japanese
  ISSN：1347-0639, J-Global ID：201302274687309054
• すざく衛星搭載広帯域全天モニタ(WAM)によるGRBの観測
  杉田聡司; 山岡和貴; 大野雅功; 高橋拓也; 深沢泰司; 洪秀徴; 阿部圭一; 遠藤康彦; 恩田香織; 田代信; 榎戸輝揚; 宮脇良平; 国分紀秀; 佐藤悟朗; 中澤知洋; 寺田幸功; 玉川徹; 高橋忠幸; 牧島一夫
  日本天文学会年会講演予稿集, Volume：2006, First page：56, 20 Feb. 2006
  Japanese
  ISSN：1347-0639, J-Global ID：201302293406120122
• 28aTF-3 GRB observation with Suzaku Wideband All-sky Monitor (HXD-WAM)　　　　　　　　　　　　　　　
  Ohno Masanori; Abe Keiichi; Endo Yasuhiko; Onda Kaori; Sato Goro; Nakazawa Kazuhiro; Takahashi Tadayuki; Enoto Teruaki; Miyawaki Ryouhei; Kokubun Motohide; Makishima Kazuo; Fukazawa Yasushi; Suzaku HXD-II team; Takahashi Takuya; Yamaoka Kazutaka; Sugita Satoshi; Terada Yukikatsu; Tamagawa Toru; Tashiro Makoto; Hong Soojing
  Meeting Abstracts of the Physical Society of Japan, Volume：61, Number：0, First page：93, Last page：93, 2006
  The Physical Society of Japan, Japanese
  ISSN：1342-8349, CiNii Articles ID：110007177175, CiNii Books ID：AA11439205
• 23aSH-9 Current Status of the Suzaku Hard X-ray Detactor Wide-band All-sky Monitor (II)　　　　　　　　　　　　　　　
  Terada Y; Suzuki M; Nakazawa K; Watanabe S; Sato G; Fukazawa Y; Mizuno T; Ohno M; Takahashi T; Kokubun M; Enoto T; Tamagawa T; Hong S; the Suzaku; HXD team; Suzuki M; Yamaoka K; Sugita S; Tashiro M; Urata Y; Abe K; Onda K
  Meeting Abstracts of the Physical Society of Japan, Volume：61, Number：0, 2006
  The Physical Society of Japan, Japanese
  CiNii Articles ID：110007179786
• 23aSH-8 Current Status of the Suzaku Hard X-ray Detector (II)　　　　　　　　　　　　　　　
  Kokubun M; Fukazawa Y; Mizuno T; Takahashi H; Tashiro S; Yamaoka K; Murakami T; Yonetoku D; the Suzaku; HXD team; Kawaharada M; Makishima K; Takahashi T; Nakazawa K; Watanabe S; Terada Y; Tamagawa T; Kubota A
  Meeting Abstracts of the Physical Society of Japan, Volume：61, Number：0, First page：74, Last page：74, 2006
  一般社団法人 日本物理学会, Japanese
  ISSN：1342-8349, CiNii Articles ID：110007183543, CiNii Books ID：AA11439205
• Strategy and early results of Suzaku gamma-ray burst observations　　　　　　　　　　　　　　　
  Tashiro, M; Suzaku GRB team
  2006
• 「すざく」衛星搭載硬X線検出器 広帯域全天モニタ部(HXD-II/WAM)の現状(I)　　　　　　　　　　　　　　　
  田代 信; 山岡和貴; 寺田幸功; 玉川 徹; 久保田あや; 牧島一夫; 国分紀秀; 高橋弘充; 釜江常好; Greg Madjeski; 深沢泰司; 水野恒史; 高橋忠幸; 中澤知洋; 渡辺伸; 村上敏夫; 米徳大輔; 能町正治; ほか「すざく」HXD チーム
  2006
• Chandra observation of the low entropy region in the radio lobe galaxy NGC 1316　　　　　　　　　　　　　　　
  M Tashiro; K Ito; K Abe; N Isobe
  PROCEEDINGS OF THE X-RAY UNIVERSE 2005, VOLS 1 AND 2, Volume：604, First page：569, Last page：+, 2006
  NGC 1316 hosts the classical double lobe radio galaxy Fornax A. Recently, Kim and Fabbiano (2003) revealed with Chandra a 'blob' like emission associated with the optical dark lane, suggesting heating by the galaxy-merging. In this paper, we show a detail analysis focusing into the 'blob' to show significantly low temperature and low entropy. The significantly lower entropy in comparison with the other inter-stellar medium structures supports that the 'blob' are produced at the past galaxy merging. Comparing with those of non-thermal electrons in the radio lobes, we discuss a possible history of the nucleus activity and show its estimated kinetic luminosity during its active phase.
  ESA PUBLICATIONS DIVISION C/O ESTEC, English
  ISSN：0379-6566, Web of Science ID：WOS:000236905300151
• Strategy and early results of Suzaku gamma-ray burst observations　　　　　　　　　　　　　　　
  Tashiro, M; Suzaku GRB team
  Advances in Space Research, 2006
• 「すざく」衛星搭載硬X線検出器 広帯域全天モニタ部(HXD-II/WAM)の現状(I)　　　　　　　　　　　　　　　
  田代 信; 山岡和貴; 寺田幸功; 玉川 徹; 久保田あや; 牧島一夫; 国分紀秀; 高橋弘充; 釜江常好; Greg Madjeski; 深沢泰司; 水野恒史; 高橋忠幸; 中澤知洋; 渡辺伸; 村上敏夫; 米徳大輔; 能町正治; ほか「すざく」HXD チーム
  日本天文学会2006年春季年会, 2006
• Preflight calibration and performance of the Astro-E2/HXD-II wide-band all-sky monitor　　　　　　　　　　　　　　　
  M Ohno; Y Fukazawa; K Yamaoka; M Kokubun; Y Terada; J Kotoku; Y Okada; S Hong; M Mori; A Tsutsui; Y Endo; K Makishima; T Murakami; K Nakazawa; T Takahashi; M Tashiro
  IEEE TRANSACTIONS ON NUCLEAR SCIENCE, Volume：52, Number：6, First page：2758, Last page：2764, Dec. 2005
  The hard X-ray detector (HXD-II) onboard Astro-E2 consists of a main detector with energy range 10-600 keV and a BGO active shield detector for background reduction. The shield detector wide-band all-sky monitor (WAM) has been designed not only for background reduction but also for all sky monitoring of gamma-ray bursts (GRB) and bright soft gamma-ray sources. WAM has a large geometrical structure of BGO scintillators for reinforcing its stopping power and has an asymmetric shape for reducing its weight. This particular structure of WAM makes the gamma-ray response very complicated, and thus we need careful calibrations before the launch. We then performed preflight calibrations of WAM as a part of the HXD-II calibrations in 2003-2004. We measured the pulse height spectra and stopping power of each unit counter individually before the HXD-II integration by exposing them to collimated gamma-rays. After integration of the HXD-II detector and installing it to the spacecraft, we measured the same issues as above for WAM by irradiating the gamma-ray source from various directions. Taking into account these experimental results, we constructed the gamma-ray response matrix of WAM using the Geant4 Monte Carlo simulation. The response developed in this work was found to have reproduced the experimental data within 10-20% accuracy.
  IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC, English
  DOI：https://doi.org/10.1109/TNS.2005.860172
  DOI ID：10.1109/TNS.2005.860172, ISSN：0018-9499, CiNii Articles ID：80019338184, Web of Science ID：WOS:000235371900007
• Development of the HXD-II wide-band all-sky monitor onboard Astro-E2　　　　　　　　　　　　　　　
  K Yamaoka; M Ohno; Y Terada; S Hong; J Kotoku; Y Okada; A Tsutsui; Y Endo; K Abe; Y Fukazawa; S Hirakuri; T Hiruta; K Itoh; T Itoh; T Kamae; M Kawaharada; N Kawano; K Kawashima; T Kishishita; T Kitaguchi; M Kokubun; GM Madejski; K Makishima; T Mitani; R Miyawaki; T Murakami; MM Murashima; K Nakazawa; H Niko; M Nomachi; K Oonuki; G Sato; M Suzuki; H Takahashi; Takahashi, I; T Takahashi; S Takeda; K Tamura; T Tanaka; M Tashiro; S Watanabe; T Yanagida; D Yonetoku
  IEEE TRANSACTIONS ON NUCLEAR SCIENCE, Volume：52, Number：6, First page：2765, Last page：2772, Dec. 2005
  The hard X-ray detector (HXD-II) is one of the three scientific instruments onboard Japanese X-ray astronomy satellite Astro-E2 scheduled to be launched in 2005. This mission is very unique in a point of having a lower background than any other past missions in the 10-600 keV range. In the HXD-II, the large and thick BGO crystals are used as active shields for particle and gamma-ray background to the main detector. They have a wide field of view of similar to 2 pi and a large effective area of 400 cm(2) even at 1 MeV. Hence, the BGO shields have been developed as a wide-band all-sky monitor (WAM) with a broadband coverage of 50-5000 keV. In this paper, overall design and performance of the HXD-II/WAM based on the results of preflight calibration tests carried out in June 2004 are described. By irradiating various radio isotopes with the WAM flight model, we verified that it had comparable capabilities with other gamma-ray burst detectors.
  IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC, English
  DOI：https://doi.org/10.1109/TNS.2005.862778
  DOI ID：10.1109/TNS.2005.862778, ISSN：0018-9499, Web of Science ID：WOS:000235371900008
• Design and performance of the soft gamma-ray detector for the NeXT mission　　　　　　　　　　　　　　　
  H Tajima; T Kamae; G Madejski; Mitani, I; K Nakazawa; T Tanaka; T Takahashi; S Watanabe; Y Fukazawa; T Ikagawa; J Kataoka; M Kokubun; K Makishima; Y Terada; M Nomachi; M Tashiro
  IEEE TRANSACTIONS ON NUCLEAR SCIENCE, Volume：52, Number：6, First page：2749, Last page：2757, Dec. 2005
  The soft gamma-ray detector (SGD) onboard the Japanese future high energy astrophysics mission (NeXT) is a Compton telescope with narrow field of view, which utilizes Compton kinematics to enhance its background rejection capabilities. It is realized as a hybrid semiconductor gamma-ray detector which consists of silicon and cadmium telluride (CdTe) detectors. It can detect photons in a wide energy band (0.05-1 MeV) at a background level of 5 x 10(-7) counts/s/cm(2) /keV; the silicon layers are required to improve the performance at a lower energy band (< 0.3 MeV). Excellent energy resolution is the key feature of the SGD, allowing it to achieve both high angular resolution and good background rejection capability. An additional capability of the SGD, its ability to measure gamma-ray polarization, opens up a new window to study properties of astronomical objects. We will present the development of key technologies to realize the SGD: high quality CdTe, low noise front-end application-specific integrated circuit, and bump bonding technology. Energy resolutions of 1.7 keV (full-width at half-maximum) for CdTe pixel detectors and 1.1 keV for Si strip detectors have been measured. We also present the validation of Monte Carlo simulation used to evaluate the performance of the SGD.
  IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC, English
  DOI：https://doi.org/10.1109/TNS.2005.862776
  DOI ID：10.1109/TNS.2005.862776, ISSN：0018-9499, CiNii Articles ID：120001466789, Web of Science ID：WOS:000235371900006
• The XMM-Newton detection of diffuse inverse compton X-rays from lobes of the FR II radio galaxy 3C 98　　　　　　　　　　　　　　　
  N Isobe; K Makishima; M Tashiro; S Hong
  ASTROPHYSICAL JOURNAL, Volume：632, Number：2, First page：781, Last page：787, Oct. 2005
  The XMM-Newton observation of the nearby FR II radio galaxy 3C 98 is reported. In two exposures on the target, faint diffuse X-ray emission associated with the radio lobes was significantly detected together with a bright X-ray active nucleus, of which the 2-10 keV intrinsic luminosity is (4-8) x 10(42) ergs s(-1). The EPIC spectra of the northern and southern lobes are reproduced by a single power-law model modified by the Galactic absorption, with a photon index of 2.2(-0.5)(+0.6) and 1.7(-0.6)(+0.7), respectively. These indices are consistent with that of the radio synchrotron spectrum, 1.73 +/- 0.01. The luminosities of the northern and southern lobes are measured to be 8.3(-2.6)(+3.3) x 10(40) and 9.2+(5.7)(-4.3) x 10(40) ergs s(-1), respectively, in the 0.7-7 keV range. The diffuse X-ray emission is interpreted as an inverse Compton emission, produced when the synchrotron-emitting energetic electrons in the lobes scatter off the cosmic microwave background photons. The magnetic field in the lobes is calculated to be about 1.7 mu G, which is about 2.5 times lower than the value estimated under the minimum energy condition. It is inferred that the energy density of the electrons exceeds that in the magnetic fields by a factor of 40-50.
  UNIV CHICAGO PRESS, English
  DOI：https://doi.org/10.1086/444341
  DOI ID：10.1086/444341, ISSN：0004-637X, Web of Science ID：WOS:000232569100008
• A short gamma-ray burst apparently associated with an elliptical galaxy at redshift z=0.225　　　　　　　　　　　　　　　
  N Gehrels; CL Sarazin; PT O'Brien; B Zhang; L Barbier; SD Barthelmy; A Blustin; DN Burrows; J Cannizzo; Cummings, JR; M Goad; ST Holland; CP Hurkett; JA Kennea; A Levan; CB Markwardt; KO Mason; P Meszaros; M Page; DM Palmer; E Rol; T Sakamoto; R Willingale; L Angelini; A Beardmore; PT Boyd; A Breeveld; S Campana; MM Chester; G Chincarini; LR Cominsky; G Cusumano; M de Pasquale; EE Fenimore; P Giommi; C Gronwall; D Grupe; JE Hill; D Hinshaw; J Hjorth; D Hullinger; KC Hurley; S Klose; S Kobayashi; C Kouveliotou; HA Krimm; Mangano, V; FE Marshall; K McGowan; A Moretti; RF Mushotzky; K Nakazawa; JP Norris; JA Nousek; JP Osborne; K Page; AM Parsons; S Patel; M Perri; T Poole; P Romano; PWA Roming; S Rosen; G Sato; P Schady; AP Smale; J Sollerman; R Starling; M Still; M Suzuki; G Tagliaferri; T Takahashi; M Tashiro; J Tueller; AA Wells; NE White; RAMJ Wijers
  NATURE, Volume：437, Number：7060, First page：851, Last page：854, Oct. 2005
  Gamma-ray bursts (GRBs) come in two classes(1): long (> 2 s), soft-spectrum bursts and short, hard events. Most progress has been made on understanding the long GRBs, which are typically observed at high redshift ( z approximate to 1) and found in subluminous star-forming host galaxies. They are likely to be produced in core-collapse explosions of massive stars(2). In contrast, no short GRB had been accurately (< 1000) and rapidly ( minutes) located. Here we report the detection of the X-ray afterglow from - and the localization of - the short burst GRB 050509B. Its position on the sky is near a luminous, non-star-forming elliptical galaxy at a redshift of 0.225, which is the location one would expect(3,4) if the origin of this GRB is through the merger of neutron-star or blackhole binaries. The X-ray afterglow was weak and faded below the detection limit within a few hours; no optical afterglow was detected to stringent limits, explaining the past difficulty in localizing short GRBs.
  NATURE PUBLISHING GROUP, English
  DOI：https://doi.org/10.1038/nature04142
  DOI ID：10.1038/nature04142, ISSN：0028-0836, PubMed ID：16208363, Web of Science ID：WOS:000232338600038
• Astro‐E2衛星の現状:硬X線検出器HXD
  中澤知洋; 釜江常好; 国分紀秀; 高橋忠幸; 高橋弘充; 田代信; 寺田幸功; 能町正治; 深沢泰司; 牧島一夫; 水野恒史; 村上敏夫; 山岡和貴; 米徳大輔; 渡辺伸; MADEJSKI Greg
  日本天文学会年会講演予稿集, Volume：2005, First page：312, 20 Aug. 2005
  Japanese
  ISSN：1347-0639, J-Global ID：201302294454175180
• 15aSA-13 Status report of the Hard X-ray detector(HXD-II) onboard Astro-E2 satellite III : Wideband All-sky Monitor(WAM) part　　　　　　　　　　　　　　　
  Yamaoka Kazutaka; Kamae Tsuneyoshi; Kokubun Norihide; Takahashi Tadayuki; Takahashi Hiromitsu; Tashiro Makoto; Terada Yukikatsu; Nakazawa Kazuhiro; Nomachi Masaharu; Fukazawa Yasushi; Makishima Kazuo; Mizuno Tsunefumi; Murakami Toshio; Watanabe Shin; Madejski Greg; on behalf of Astro-E2 HXD-II team
  Meeting abstracts of the Physical Society of Japan, Volume：60, Number：2, First page：37, Last page：37, 19 Aug. 2005
  The Physical Society of Japan (JPS), Japanese
  ISSN：1342-8349, CiNii Articles ID：110004558749, CiNii Books ID：AA11439205
• 14aSF-9 WIDGET(WIDe-field telescope GRB for Early Timing) STATUS　　　　　　　　　　　　　　　
  Abe K.; Tamagawa T.; Usui F.; Terada Y.; Urata Y.; Onda K.; Tashiro M.; Azuma H.; Kuwahara M.; the WIDGET team
  Meeting abstracts of the Physical Society of Japan, Volume：60, Number：2, First page：29, Last page：29, 19 Aug. 2005
  The Physical Society of Japan (JPS), Japanese
  ISSN：1342-8349, CiNii Articles ID：110004558724, CiNii Books ID：AA11439205
• 14aSF-6 Connection between X-ray early afterglow and prompt emission observed by Swift GRB Explorer　　　　　　　　　　　　　　　
  Sato Goro; Takahashi Tadayuki; Nakazawa Kazuhiro; Mitani Takefumi; Tashiro Makoto; Suzuki Masaya; Gehrels Neil; Hullinger Derek; Parsons Ann; Sakamoto Takanori; the Swift team
  Meeting abstracts of the Physical Society of Japan, Volume：60, Number：2, First page：29, Last page：29, 19 Aug. 2005
  The Physical Society of Japan (JPS), Japanese
  ISSN：1342-8349, CiNii Articles ID：110004558722, CiNii Books ID：AA11439205
• 15aSA-11 Current Status of the Astro-E2 Hard X-ray Detector : I　　　　　　　　　　　　　　　
  Kokubun N.; Kamae T.; Takahashi T.; Takahashi H.; Tashiro S.; Terada Y.; Nakazawa K.; Nomachi M.; Fukaawa Y.; Makishima K.; Mizuno T.; Murakami T.; Yamaoka K.; Watanabe S.; Yonetoku D.; Madejski Greg; and HXD-II team
  Meeting abstracts of the Physical Society of Japan, Volume：60, Number：2, First page：37, Last page：37, 19 Aug. 2005
  The Physical Society of Japan (JPS), Japanese
  ISSN：1342-8349, CiNii Articles ID：110004558748, CiNii Books ID：AA11439205
• 14aSF-5 Status of the Gamma-Ray Burst Observatory Swift　　　　　　　　　　　　　　　
  Tashiro Makoto; Takahashi Tadayuki; Nakazawa Kazuhiro; Sato Goro; Suzuki Masaya; Mitani Takefumi; Gehrels Neil; the Swift team
  Meeting abstracts of the Physical Society of Japan, Volume：60, Number：2, First page：29, Last page：29, 19 Aug. 2005
  The Physical Society of Japan (JPS), Japanese
  ISSN：1342-8349, CiNii Articles ID：110004558721, CiNii Books ID：AA11439205
• Hard x-ray response of CdZnTe detectors in the swift burst alert telescope　　　　　　　　　　　　　　　
  M Suzuki; M Tashiro; G Sato; S Watanabe; K Nakazawa; T Takahashi; Y Okada; H Takahashi; A Parsons; S Barthelmy; J Cummings; N Gehrels; D Hullinger; H Krimm; J Tueller
  IEEE TRANSACTIONS ON NUCLEAR SCIENCE, Volume：52, Number：4, First page：1033, Last page：1035, Aug. 2005
  The Burst Alert Telescope (BAT) onboard the Swift gamma-ray burst explorer has a coded aperture mask and a detector array of 32 K CdZnTe semiconductor devices. Due to the small mobility and short lifetime of carriers, the electron-hole pairs generated by gamma-ray irradiation cannot be fully collected. Hence the shape of the measured spectra has a broad low-energy tail. We have developed a method to model the spectral response by taking into account the charge transport properties which depend on the depth of the photon interaction [1]. The mobility-lifetime products for detectors derived from our method vary by more than one order of magnitude among detectors. In this paper, we focus on the nonuniformity of the mobility at the millimeter scale by employing a scanning experiment for a single detector. We reveal almost an order of magnitude variance in the mobility-lifetime product of holes within a single detector, while those of electrons, remains fairly uniform.
  IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC, English
  DOI：https://doi.org/10.1106/TNS.2005.0852968
  DOI ID：10.1106/TNS.2005.0852968, ISSN：0018-9499, Web of Science ID：WOS:000231436700033
• Development of a Monte Carlo simulator for the Astro-E2 Hard X-ray Detector (HXD-II)　　　　　　　　　　　　　　　
  Y Terada; S Watanabe; M Ohno; M Suzuki; T Itoh; Takahashi, I; G Sato; M Murashima; N Kawano; Y Uchiyama; S Kubo; T Takahashi; M Tashiro; M Kokubun; K Makishima; T Kamae; T Murakami; M Nomachi; Y Fukazawa; K Yamaoka; K Nakazawa; D Yonetoku
  IEEE TRANSACTIONS ON NUCLEAR SCIENCE, Volume：52, Number：4, First page：902, Last page：909, Aug. 2005
  The Hard X-ray Detector (HXD-II) is one of the scientific payloads on board the fifth Japanese cosmic X-ray satellite Astro-E2, scheduled for launch in 2005. The HXD-II is designed to cover a wide energy range of 10-600 keV with a high sensitivity of about 10(-5) cnt/s/cm(2) /keV. In order to derive the energy response of the sensor and to estimate the background, a Monte Carlo simulator based on the Geant4 toolkit is currently being developed. This paper describes the design concept of the HXD-II software package, including the analysis tools and the Monte Carlo simulator, and its verification through a comparison with actual data taken by pre-flight radio-isotope irradiation experiments, together with calculated outputs that can demonstrate the in-orbit performance of the HXD-II.
  IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC, English
  DOI：https://doi.org/10.1109/TNS.2005.852681
  DOI ID：10.1109/TNS.2005.852681, ISSN：0018-9499, CiNii Articles ID：80017820078, Web of Science ID：WOS:000231436700014
• The search for optical emission on and before the GRB trigger with the WIDGET telescope　　　　　　　　　　　　　　　
  T Tamagawa; F Usui; Y Urata; K Abe; K Onda; M Tashiro; Y Terada; H Fujiwara; N Miura; S Hirose; N Kawai; A Yoshida; M Mori; K Makishima
  NUOVO CIMENTO DELLA SOCIETA ITALIANA DI FISICA C-COLLOQUIA ON PHYSICS, Volume：28, Number：4-5, First page：771, Last page：774, Jul. 2005
  WIDGET is a robotic telescope for rnonitoring the HETE-2 field-of-view to detect Gamma-Ray Burst optical flashes or possible optical precursors. The system has 62 degrees x 62 degrees wide field-of-view which covers about 80% of HETE-2 one with a, 2kx2k Apogee U10 CCD camera and a Canon EF 24 mm f/1.4 wide-angle lens without a bandpass filter. WIDGET has been in operation since June 2004 at Akeno observing site where is about 200 kin apart from Tokyo. Typical limiting magnitude with S/N=3 at the site is V = 10(mag) for 5 seconds exposure and V = 11(mag) for 30 seconds exposure. We had already six coincident observations with HETE-2 position alerts. It was, however, cloudy for all cases due to rainy season in Japan. The expected number of coincident observations under clear sky is about 5 events per year. We will extend the system in early 2005 for Swift era to monitor optical transients in wider field-of-view, multi-color or polarization modes.
  SOC ITALIANA FISICA, English
  DOI：https://doi.org/10.1393/ncc/i2005-10150-1
  DOI ID：10.1393/ncc/i2005-10150-1, ISSN：1124-1896, Web of Science ID：WOS:000234266300063
• Performance of GRB monitor with Astro-E2 Hard X-ray Detector (HXD-II)　　　　　　　　　　　　　　　
  S Hong; K Yamaoka; Y Terada; A Ohno; A Tsutsui; Y Endo; J Kotoku; Y Okada; A Mori; Y Fukazawa; T Kamae; M Kokubun; K Makishima; T Murakami; K Nakazawa; M Nomachi; M Tashiro; Takahashi, I; T Takahashi; D Yonetoku; S Watanabe
  NUOVO CIMENTO DELLA SOCIETA ITALIANA DI FISICA C-COLLOQUIA ON PHYSICS, Volume：28, Number：4-5, First page：821, Last page：824, Jul. 2005
  The Hard X-ray Detector (HXD-II) is one of the three instruments onboard the Astro-E2 satellite scheduled for launch in 2005. The HXD-II consists of 16 main counters (Well units), surrounded by 20 active shield counters (Anti units). The Anti units have a large geometrical area of similar to 800 cm(2) with an uncollimated field of view covering similar to 2 pi steradian. Utilizing 2.6 cm thick BGO crystals: they realize a large effective area of 400 cm(2) for 1 MeV photons. In the energy range of 300-5000 keV, the expected effective area is significantly larger than those of other gamma-ray burst instruments, such as CGRO/BATSE, HETE-2/FREGATE, and GLAST/GBM. Therefore. the Anti units act as a Wideband All-sky, Monitor (WAM) for gamma-ray bursts in the energy range of 50-5000 keV.
  SOC ITALIANA FISICA, English
  DOI：https://doi.org/10.1393/ncc/i2005-10164-7
  DOI ID：10.1393/ncc/i2005-10164-7, ISSN：1124-1896, Web of Science ID：WOS:000234266300074
• Development of a spectral model based on charge transport for the Swift/BAT 32K CdZnTe detector array　　　　　　　　　　　　　　　
  G Sato; A Parsons; D Hullinger; M Suzuki; T Takahashi; M Tashiro; K Nakazawa; Y Okada; H Takahashi; S Watanabe; S Barthelmy; J Cummings; N Gehrels; H Krimm; C Markwardt; J Tueller; E Fenimore; D Palmer
  NUCLEAR INSTRUMENTS & METHODS IN PHYSICS RESEARCH SECTION A-ACCELERATORS SPECTROMETERS DETECTORS AND ASSOCIATED EQUIPMENT, Volume：541, Number：1-2, First page：372, Last page：384, Apr. 2005
  The properties of 32K CdZnTe (4 x 4 mm(2) large, 2 rum thick) detectors have been studied in the pre-flight calibration of the Burst Alert Telescope (BAT) on-board the Swift Gamma-ray Burst Explorer (scheduled for launch in November 2004). In order to understand the energy response of the BAT CdZnTe array, we first quantify the mobility-lifetime (mu tau) products of carriers in individual CdZnTe detectors, which produce a position dependency in the charge induction efficiency and results in a low-energy tail in the energy spectrum. Based on a new method utilizing Co-57 spectra obtained at different bias voltages, the mu tau for electrons ranges from 5.0 x 10(-4) to 1.0 x 10(-2) cm(2) V-1 while the mu tau for holes ranges from 1.3 x 10(-5) to 1.8 x 10(-4) cm(2) V-1. We find that this wide distribution of mu tau products explains the large diversity in spectral shapes between CdZnTe detectors well. We also find that the variation of mu tau products can be attributed to the difference of crystal ingots or manufacturing harness. We utilize the 32K sets of extracted mu tau products to develop a spectral model of the detector. In combination with Monte Carlo simulations, we can construct a spectral model for any photon energy or any incident angle. (c) 2005 Elsevier B.V. All rights reserved.
  ELSEVIER SCIENCE BV, English
  DOI：https://doi.org/10.1016/j.nima.2005.01.078
  DOI ID：10.1016/j.nima.2005.01.078, ISSN：0168-9002, Web of Science ID：WOS:000228620600048
• Application of CdTe for the NeXT mission　　　　　　　　　　　　　　　
  T Takahashi; K Nakazawa; S Watanabe; G Sato; T Mitani; T Tanaka; K Oonuki; K Tamura; H Tajima; T Kamae; G Madejski; M Nomachi; Y Fukazawa; K Makishima; M Kokubun; Y Terada; J Kataoka; M Tashiro
  NUCLEAR INSTRUMENTS & METHODS IN PHYSICS RESEARCH SECTION A-ACCELERATORS SPECTROMETERS DETECTORS AND ASSOCIATED EQUIPMENT, Volume：541, Number：1-2, First page：332, Last page：341, Apr. 2005
  Cadmium telluride (CdTe) and cadmium zinc telluride (CdZnTe) have been regarded as promising semiconductor materials for hard X-ray and gamma-ray detection. The high-atomic number of the materials (Z(Cd) = 48, Z(Te) = 52) gives a high quantum efficiency in comparison with Si. The large band-gap energy (E-g = 1.5 eV) allows to operate the detector at room temperature. Based on recent achievements in high-resolution CdTe detectors, in the technology of ASICs and in bump-bonding, we have proposed the novel hard X-ray and gamma-ray detectors for the NeXT mission in Japan. The high-energy response of the super mirror onboard NeXT will enable us to perform the first sensitive imaging observations up to 80keV. The focal plane detector, which combines a fully depleted X-ray CCD and a pixellated CdTe detector, will provide spectra and images in the wide energy range from 0.5 to 80keV. In the soft gamma-ray band up to similar to 1 MeV, a narrow field-of-view Compton gamma-ray telescope utilizing several tens of layers of thin Si or CdTe detector will provide precise spectra with much higher sensitivity than present instruments. The continuum sensitivity will reach several x 10(-8) photons(-1) keV(-1) cm(-1) in the hard X-ray region and a few X 10(-7) photons(-1) keV(-1) cm(-2) in the soft gamma-ray region. (c) 2005 Elsevier B.V. All rights reserved.
  ELSEVIER SCIENCE BV, English
  DOI：https://doi.org/10.1016/0j.nima.2005.01.073
  DOI ID：10.1016/0j.nima.2005.01.073, ISSN：0168-9002, Web of Science ID：WOS:000228620600043
• The swift gamma-ray burst mission (vol 611, pg 1005, 2004)　　　　　　　　　　　　　　　
  N Gehrels; G Chincarini; P Giommi; KO Mason; JA Nousek; AA Wells; NE White; SD Barthelmy; DN Burrows; LR Cominsky; KC Hurley; FE Marshall; P Meszaros; PWA Roming; L Angelini; LM Barbier; T Belloni; PT Boyd; S Campana; PA Caraveo; MM Chester; O Citterio; TL Cline; MS Cropper; Cummings, JR; AJ Dean; ED Feigelson; EE Fenimore; DA Frail; AS Fruchter; GP Garmire; K Gendreau; G Ghisellini; J Greiner; JE Hill; SD Hunsberger; HA Krimm; Kulkarni, SR; P Kumar; F Lebrun; NM Lloyd-Ronning; CB Markwardt; BJ Mattson; RF Mushotzky; JP Norris; B Paczynski; DM Palmer; HS Park; AM Parsons; J Paul; MJ Rees; CS Reynolds; JE Rhoads; TP Sasseen; BE Schaefer; AT Short; AP Smale; IA Smith; L Stella; M Still; G Tagliaferri; T Takahashi; M Tashiro; LK Townsley; J Tueller; MJL Turner; M Vietri; W Voges; MJ Ward; R Willingale; FM Zerbi; WW Zhang
  ASTROPHYSICAL JOURNAL, Volume：621, Number：1, First page：558, Last page：558, Mar. 2005
  IOP PUBLISHING LTD, English, Others
  ISSN：0004-637X, Web of Science ID：WOS:000227406200052
• Astro‐E2衛星硬X線検出器(HXD‐II)のソフトウェア開発の現状
  寺田幸功; 渡辺伸; 尾崎正伸; 大野雅功; 鈴木雅也; 伊藤健; 内山泰伸; 久保信; 佐藤悟朗; 高橋勲; 川原田円; 村島未生; 宮脇良平; 柳田健之; 三谷烈史; 田中孝明; 川埜直美; 洪秀徴; 牧島一夫; 高橋忠幸; 村上敏夫; 田代信; 深沢泰司; 国分紀秀; 中澤知洋; 山岡和貴; 米徳大輔
  日本天文学会年会講演予稿集, Volume：2005, First page：251, 20 Feb. 2005
  Japanese
  ISSN：1347-0639, J-Global ID：201302296356632096
• Swift衛星搭載BAT検出器の軌道上における性能評価
  鈴木雅也; 田代信; 佐藤悟朗; 中澤知洋; 高橋忠幸; 岡田祐; 高橋弘充; BARTHELMY Scott; CUMMINGS Jay; GEHRELS Neil; HULLINGER Derek; KRIMM Hans; MARKWARDT Craig; PARSONS Ann; 坂本貴紀; TULLER Jack; DEAN Tony; WILLIS Dave
  日本天文学会年会講演予稿集, Volume：2005, First page：256, 20 Feb. 2005
  Japanese
  ISSN：1347-0639, J-Global ID：201302275773126864
• Swift衛星の運用状況とガンマ線バースト観測の初期成果
  佐藤悟朗; 高橋忠幸; 中澤知洋; 田代信; 鈴木雅也; 岡田祐; 高橋弘充; BARTHELMY Scott; CUMMINGS Jay; GEHRELS Neil; HULLINGER Derek; KRIMM Hans; MARKWARDT Craig; PARSONS Ann; 坂本貴紀; TULLER Jack
  日本天文学会年会講演予稿集, Volume：2005, First page：255, 20 Feb. 2005
  Japanese
  ISSN：1347-0639, J-Global ID：201302276453576744
• ガンマ線バースト観測衛星Swiftの現状　　　　　　　　　　　　　　　
  田代 信; 鈴木 雅也; 佐藤 悟朗
  Volume：5, First page：730, Last page：733, 06 Jan. 2005
  Japanese
  CiNii Articles ID：40007317008, CiNii Books ID：AA11571712
• Chandra observation of the low entropy region in the radio lobe galaxy NGC 1316　　　　　　　　　　　　　　　
  Tashiro, M; Ito, K; Abe, K; Isobe, N
  The X-ray Universe, First page：261, Last page：261, 2005
• The burst alert telescope (BAT) on the Swift MIDEX mission　　　　　　　　　　　　　　　
  SD Barthelmy; LM Barbier; Cummings, JR; EE Fenimore; N Gehrels; D Hullinger; HA Krimm; CB Markwardt; DM Palmer; A Parsons; G Sato; M Suzuki; T Takahashi; M Tashiro; J Tueller
  SPACE SCIENCE REVIEWS, Volume：120, Number：3-4, First page：143, Last page：164, 2005
  The burst alert telescope (BAT) is one of three instruments on the Swift MIDEX spacecraft to study gamma-ray bursts (GRBs). The BAT first detects the GRB and localizes the burst direction to an accuracy of 1-4 arcmin within 20s after the start of the event. The GRB trigger initiates an autonomous spacecraft slew to point the two narrow field-of-view (FOV) instruments at the burst location within 20-70 s so to make follow-up X-ray and optical observations. The BAT is a wide-FOV, coded-aperture instrument with a CdZnTe detector plane. The detector plane is composed of 32,768 pieces of CdZnTe (4x4x2 mm), and the coded-aperture mask is composed of similar to 52,000 pieces of lead (5x5x1 mm) with a 1-m separation between mask and detector plane. The BAT operates over the 15-150 keV energy range with similar to 7 keV resolution, a sensitivity of similar to 10(-8) ergg s(-1) cm(-2), and a 1.4 sr (half-coded) FOV. We expect to detect >100 GRBs/year for a 2-year mission. The BAT also performs an all-sky hard X-ray survey with a sensitivity of similar to 2 m Crab (systematic limit) and it serves as a hard X-ray transient monitor.
  SPRINGER, English, Book review
  DOI：https://doi.org/10.1007/s11214-005-5096-3
  DOI ID：10.1007/s11214-005-5096-3, ISSN：0038-6308, Web of Science ID：WOS:000235280600002
• Development and qualification of the HXD-II onboard Astro-E2
  Madoka Kawaharada; Soojing Hong; Mio M. Murashima; Motohide Kokubun; Takeshi Itoh; Kazuo Makishima; Ryouhei Miyawaki; Hisako Niko; Takayuki Yanagida; Takefumi Mitani; Kazuhiro Nakazawa; Kousuke Oonuki; Tadayuki Takahashi; Ken'ichi Tamura; Takaaki Tanaka; Yukikatsu Terada; Yasushi Fukazawa; Naomi Kawano; Kengo Kawashima; Masanori Ohno; Kazutaka Yamaoka; Keiichi Abe; Masaya Suzuki; Makoto Tashiro; Daisuke Yonetoku; Toshio Murakami
  Proceedings of SPIE - The International Society for Optical Engineering, Volume：5501, First page：286, Last page：295, 01 Dec. 2004
  The Hard X-ray Detector (HXD-II), one of instruments onboard the Astro-E2 satellite to be launched in February 2005, is in the final stage of its development. The HXD-II probes the universe in the energy range of 10-600 keV with a sensitivity by an order of magnitude better than those of previous missions. The assembly of the HXD-II completed in January 2004, followed by a series of pre-launch qualification tests. As a result, the design goals of the HXD-II have been met. These include; a background level of 5 × 10 -6 counts/s/keV/cm 2 at 200 keV for GSO and 1 × 10 -5 counts/s/keV/cm 2 at 30 keV for PIN; energy resolutions of 2.9 keV (PIN diode, at 59.5 keV) and 10 % (GSO scintillator, at 662 keV); and low energy thresholds of 10 keV for PIN diodes and 30 keV for GSO scintillators. The measured background predicts a continuum sensitivity of a few ×10 -6 photons/s/keV/cm 2 . Anti-Counter units surrounding the HXD-II provide 50 keV-5 MeV information on gamma-ray bursts and bright X-ray transients.
  DOI：https://doi.org/10.1117/12.551051
  DOI ID：10.1117/12.551051, ISSN：0277-786X, SCOPUS ID：19944367586
• Design and performance of soft Gamma-ray detector for NeXT mission　　　　　　　　　　　　　　　
  H. Tajima; T. Kamae; G. Madejski; T. Mitani; K. Nakazawa; T. Tanaka; T. Takahashi; S. Watanabe; Y. Fukazawa; T. Ikagawa; J. Kataoka; M. Kokubun; K. Makishima; Y. Terada; M. Nomachi; M. Tashiro
  IEEE Nuclear Science Symposium Conference Record, Volume：1, First page：314, Last page：321, 01 Dec. 2004
  The Soft Gamma-ray Detector (SGD) on board NeXT (Japanese future high energy astrophysics mission) is a Compton telescope with narrow field of view (FOV), which utilizes Compton kinematics to enhance its background rejection capabilities. It is realized as a hybrid semiconductor gamma-ray detector which consists of silicon and CdTe (Cadmium Telluride) detectors. It can detect photons in a wide energy band (0.05-1 MeV) at a background level of 5 × 10-7counts/s/cm2/keV; the silicon layers are required to improve the performance at a lower energy band (<0.3 MeV). Excellent energy resolution is the key feature of the SGD, allowing to achieve both high angular resolution and good background rejection capability. An additional capability of the SGD, its ability to measure gamma-ray polarization opens up a new window to study properties of astronomical objects. We will present the development of key technologies to realize the SGD; high quality CdTe, low noise front-end ASIC and bump bonding tecnology. Energy resolutions of 1.7 keV (FWHM) for CdTe pixel detectors and 1.1 keV for Si strip detectors have been measured. We also present the validation of MC simulation used to evaluate the performance of the SGD. © 2004 IEEE.
  Scopus Citedby：https://www.scopus.com/inward/citedby.uri?partnerID=HzOxMe3b&scp=23844483540&origin=inward
  ISSN：1095-7863, SCOPUS ID：23844483540
• 28aSD-8 PreFlight Calibration and Performance of the Astro-E2/HXD-II Anti Counter as the All Sky Monitor　　　　　　　　　　　　　　　
  Ohno Masanori; Fukazawa Yasushi; Yamaoka Kazutaka; Tsutsui Akihito; Makishima Kazuo; Kokubun Motohide; Terada Yukikatsu; Kotoku Junichi; Tashiro Makoto; Hong Soojing; Mori Masanori; Murakami Toshio; Takahashi Tadayuki; Nakazawa Kazuhiro
  Meeting abstracts of the Physical Society of Japan, Volume：59, Number：2, First page：76, Last page：76, 25 Aug. 2004
  The Physical Society of Japan (JPS), Japanese
  ISSN：1342-8349, CiNii Articles ID：110002050716, CiNii Books ID：AA11439205
• 28pSD-11 The search for optical emission on and before the GRB with the WIDGET　　　　　　　　　　　　　　　
  Abe K; Tamagawa T; Usui F; Terada Y; Urata Y; Onda K; Tashiro M; Fujiwara H; Miura N; Hirose S; Makishima K; Mori M; Kawai N; Yoshida A
  Meeting abstracts of the Physical Society of Japan, Volume：59, Number：2, First page：80, Last page：80, 25 Aug. 2004
  The Physical Society of Japan (JPS), Japanese
  ISSN：1342-8349, CiNii Articles ID：110002050772, CiNii Books ID：AA11439205
• The Swift gamma-ray burst mission　　　　　　　　　　　　　　　
  N Gehrels; G Chincarini; P Giommi; KO Mason; JA Nousek; AA Wells; NE White; SD Barthelmy; DN Burrows; LR Cominsky; KC Hurley; FE Marshall; P Meszaros; PWA Roming; L Angelini; LM Barbier; T Belloni; S Campana; PA Caraveo; MM Chester; O Citterio; TL Cline; MS Cropper; Cummings, JR; AJ Dean; ED Feigelson; EE Fenimore; DA Frail; AS Fruchter; GP Garmire; K Gendreau; G Ghisellini; J Greiner; JE Hill; SD Hunsberger; HA Krimm; Kulkarni, SR; P Kumar; F Lebrun; NM Lloyd-Ronning; CB Markwardt; BJ Mattson; RF Mushotzky; JP Norris; J Osborne; B Paczynski; DM Palmer; HS Park; AM Parsons; J Paul; MJ Rees; CS Reynolds; JE Rhoads; TP Sasseen; BE Schaefer; AT Short; AP Smale; IA Smith; L Stella; G Tagliaferri; T Takahashi; M Tashiro; LK Townsley; J Tueller; MJL Turner; M Vietri; W Voges; MJ Ward; R Willingale; FM Zerbi; WW Zhang
  ASTROPHYSICAL JOURNAL, Volume：611, Number：2, First page：1005, Last page：1020, Aug. 2004
  The Swift mission, scheduled for launch in 2004, is a multiwavelength observatory for gamma-ray burst (GRB) astronomy. It is a first-of-its-kind autonomous rapid-slewing satellite for transient astronomy and pioneers the way for future rapid-reaction and multiwavelength missions. It will be far more powerful than any previous GRB mission, observing more than 100 bursts yr(-1) and performing detailed X-ray and UV/optical afterglow observations spanning timescales from 1 minute to several days after the burst. The objectives are to (1) determine the origin of GRBs, (2) classify GRBs and search for new types, (3) study the interaction of the ultrarelativistic outflows of GRBs with their surrounding medium, and (4) use GRBs to study the early universe out to z>10. The mission is being developed by a NASA-led international collaboration. It will carry three instruments: a new-generation wide-field gamma-ray (15-150 keV) detector that will detect bursts, calculate 1'-4' positions, and trigger autonomous spacecraft slews; a narrow-field X-ray telescope that will give 5" positions and perform spectroscopy in the 0.2-10 keV band; and a narrow-field UV/optical telescope that will operate in the 170-600 nm band and provide 0".3 positions and optical finding charts. Redshift determinations will be made for most bursts. In addition to the primary GRB science, the mission will perform a hard X-ray survey to a sensitivity of similar to1 mcrab (similar to2x10(-11) ergs cm(-2) s(-1) in the 15-150 keV band), more than an order of magnitude better than HEAO 1 A-4. A flexible data and operations system will allow rapid follow-up observations of all types of high-energy transients, with rapid data downlink and uplink available through the NASA TDRSS system. Swift transient data will be rapidly distributed to the astronomical community, and all interested observers are encouraged to participate in follow-up measurements. A Guest Investigator program for the mission will provide funding for community involvement. Innovations from the Swift program applicable to the future include (1) a large-area gamma-ray detector using the new CdZnTe detectors, (2) an autonomous rapid-slewing spacecraft, (3) a multiwavelength payload combining optical, X-ray, and gamma-ray instruments, (4) an observing program coordinated with other ground-based and space-based observatories, and (5) immediate multiwavelength data flow to the community. The mission is currently funded for 2 yr of operations, and the spacecraft will have a lifetime to orbital decay of similar to8 yr.
  IOP PUBLISHING LTD, English
  DOI：https://doi.org/10.1086/422091
  DOI ID：10.1086/422091, ISSN：0004-637X, eISSN：1538-4357, Web of Science ID：WOS:000223403400032
• X-rays from Radio Lobes : As a probe of the jet energetics　　　　　　　　　　　　　　　
  TASHIRO Makoto; ISOBE Naoki
  The Astronomical herald, Volume：97, Number：7, First page：400, Last page：405, 20 Jun. 2004
  Japanese
  ISSN：0374-2466, CiNii Articles ID：10013127825, CiNii Books ID：AN00154555
• 27aZE-5 Chandra and XMM-Newton observations of the radio galaxies For A and Cen B　　　　　　　　　　　　　　　
  Tashiro M; Suzuki M; Ito K; Abe K; Isobe N
  Meeting abstracts of the Physical Society of Japan, Volume：59, Number：1, First page：78, Last page：78, 03 Mar. 2004
  The Physical Society of Japan (JPS), Japanese
  ISSN：1342-8349, CiNii Articles ID：110002184488, CiNii Books ID：AA11439205
• 28aZK-6 Assembly and Calibration of the WELL detection part in the HXD-II onboard Astro-E2　　　　　　　　　　　　　　　
  Kawaharada M; Murashima M; Itoh T; Niko H; Miyawaki R; Yanagida T; kokubun M; Makishima K; Mitani T; Tanaka T; Oonuki K; Tamura K; Nakazawa K; Takahashi T; Kawano N; Kawashima K; Fukazawa Y; Suzuki M; Abe K; Tashiro M
  Meeting abstracts of the Physical Society of Japan, Volume：59, Number：1, First page：89, Last page：89, 03 Mar. 2004
  The Physical Society of Japan (JPS), Japanese
  ISSN：1342-8349, CiNii Articles ID：110002184665, CiNii Books ID：AA11439205
• Hard X-ray and gamma-ray detectors for the NeXT mission　　　　　　　　　　　　　　　
  T Takahashi; K Makishima; Y Fukazawa; M Kokubun; K Nakazawa; M Nomachi; H Tajima; M Tashiro; Y Terada
  NEW ASTRONOMY REVIEWS, Volume：48, Number：1-4, First page：269, Last page：273, Feb. 2004
  When compared with X-ray astronomy, the gamma-ray astronomy, especially in the energy band from 10 keV to several MeV, is still immature and significant improvements should be done to obtain sensitivity comparable to that achieved in the energy band below 10 keV. In order to fill this "sensitivity gap", the NeXT (New X-ray Telescope) mission has been proposed as a successor of the Astro-E2 mission. The high-energy response of the super mirror will enable us to perform first sensitive imaging observation up to 80 keV. One idea for the focal plane detector is to combine a fully depleted X-ray imaging device (soft X-ray detector) and a pixelated CdTe (cadmium telluride) detector. In the soft gamma-ray band upto similar to1 MeV, a narrow field-of-view Compton gamma-ray telescope utilizing several tens of layers of thin Si or CdTe detector has been proposed to obtain much higher sensitivity than present instruments. (C) 2003 Elsevier B.V. All rights reserved.
  ELSEVIER SCI LTD, English
  DOI：https://doi.org/10.1016/j.newar.2003.11.047
  DOI ID：10.1016/j.newar.2003.11.047, ISSN：1387-6473, Web of Science ID：WOS:000189181600048
• NeXTが目指すサイエンス:活動銀河ジェットの物理　　　　　　　　　　　　　　　
  片岡 淳; 田代 信; 深沢 泰司
  Volume：4, First page：43, Last page：46, 08 Jan. 2004
  Japanese
  CiNii Articles ID：40007259370, CiNii Books ID：AA11571712
• Astro-E2およびNeXT衛星によるガンマ線バーストの観測の可能性　　　　　　　　　　　　　　　
  米徳 大輔; 村上 敏夫; 田代 信
  Volume：4, First page：63, Last page：65, 08 Jan. 2004
  Japanese
  CiNii Articles ID：40007259375, CiNii Books ID：AA11571712
• Swift衛星搭載BAT検出器の数値モデルとエネルギー応答　　　　　　　　　　　　　　　
  鈴木 雅也; 田代 信; 佐藤 悟朗
  Volume：4, First page：463, Last page：466, 08 Jan. 2004
  Japanese
  CiNii Articles ID：40007259470, CiNii Books ID：AA11571712
• ガンマ線バースト観測衛星Swift搭載BAT検出器の数値モデルとエネルギー応答
  鈴木雅也; 田代信; 佐藤悟朗; 渡辺伸; 中澤知洋; 高橋忠幸; 岡田祐; 高橋弘充; BARTHELMY Scott; CUMMINGS Jay; GEHRELS Neil; HULLINGER Derek; KRIMM Hans; MARKWARDT Craig; PARSONS Ann; TULLER Jack; DEAN Tony; WILLIS Dave
  日本天文学会年会講演予稿集, Volume：2004, First page：262, 2004
  Japanese
  ISSN：1347-0639, J-Global ID：201302236749216580
• ガンマ線バースト観測衛星Swiftの開発の現状と観測計画
  田代信; 鈴木雅也; 高橋忠幸; 佐藤悟朗; 中澤知洋; 渡辺伸; 岡田祐; 高橋弘充; 国分紀秀; 牧島一夫; GEHRELS Neil
  日本天文学会年会講演予稿集, Volume：2004, First page：52, 2004
  Japanese
  ISSN：1347-0639, J-Global ID：201302292631407590
• Astro‐E2衛星搭載硬X線検出器(HXD‐II)主検出部の打ち上げ前較正試験
  村島未生; 川原田円; 二河久子; 宮脇良平; 高橋勲; 国分紀秀; 牧島一夫; 三谷烈史; 渡辺伸; 中澤知洋; 川埜直美; 鈴木雅也; 田代信; 寺田幸功
  日本天文学会年会講演予稿集, Volume：2004, First page：248, 2004
  Japanese
  ISSN：1347-0639, J-Global ID：201302236760898021
• Design and Performance of Digital Electronics of HXD-II　　　　　　　　　　　　　　　
  Takahashi Hiromitsu; Kokubun Motohide; Makishima Kazuo; Tashiro Makoto; Suzuki Masaya; Terada Yukikatsu; Takahashi Tadayuki; Nakazawa Kazuhiro; Fukazawa Yasushi; HXD team
  Meeting abstracts of the Physical Society of Japan, Volume：58, Number：2, First page：13, Last page：13, 15 Aug. 2003
  The Physical Society of Japan (JPS), Japanese
  ISSN：1342-8349, CiNii Articles ID：110002058382, CiNii Books ID：AA11439205
• Gurrent status of the Astro-E2 Hard X-ray Detector (2)　　　　　　　　　　　　　　　
  Kokubun M.; Makishima K.; Nakazawa K.; Takabashi T.; Fukazawa Y.; Tashiro S.; Yamaoka K.; Terada Y.; Yonetoku D.; Murakami T.; Nomachi M.; Kamae T.; HXD-H team
  Meeting abstracts of the Physical Society of Japan, Volume：58, Number：2, First page：80, Last page：80, 15 Aug. 2003
  The Physical Society of Japan (JPS), Japanese
  ISSN：1342-8349, CiNii Articles ID：110002058831, CiNii Books ID：AA11439205
• Activation properties of Schottky CdTe diodes irradiated by 150 MeV protons　　　　　　　　　　　　　　　
  MM Murakami; Y Kobayashi; M Kokubun; Takahashi, I; Y Okada; M Kawaharada; K Nakazawa; S Watanabe; G Sato; M Kouda; T Mitani; T Takahashi; M Suzuki; M Tashiro; S Kawasoe; M Nomachi; K Makishima
  IEEE TRANSACTIONS ON NUCLEAR SCIENCE, Volume：50, Number：4, First page：1013, Last page：1019, Aug. 2003
  Cadmium Telluride (CdTe), with its high photon absorption efficiency, has been regarded as a promising semiconductor material for the next generation X/gamma-ray detectors. In order to apply this device to astrophysics, it is essential to investigate the radiation hardness and background properties induced by cosmic-ray protons in orbit. We irradiated Schottky CdTe diodes and a CdTe block with a beam of mono-energetic (150 MeV) protons. The induced activation in CdTe was measured externally with a germanium detector, and internally with the irradiated CdTe diode itself. We successfully identified most of radioactive isotopes induced mainly via (p, xn) reactions, and confirmed that the activation background level of CdTe diode is sufficiently low in orbit. We compared energy resolution and leakage current before and after the irradiation and also monitored the signals from a calibration source during the irradiation. There have been no significant degradation. CdTe diodes are tolerant enough to radioactivity in low earth orbit.
  IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC, English
  DOI：https://doi.org/10.1109/TNS.2003.815120
  DOI ID：10.1109/TNS.2003.815120, ISSN：0018-9499, Web of Science ID：WOS:000184789000047
• Swift Burst Alert Telescope Calibration (2)　　　　　　　　　　　　　　　
  Suzuki M.; Tashiro M.; Sato Goro; Watanabe Shin; Nakazawa Kazuhiro; Takahashi Tadayuki; Takahashi Hiromitsu; Okada Yuu; Kokubun Motohide; Makishima Kazuo; Barthelmy Scott; Cummings Jay; Krimm Hans; Gehrels Neil; Hullinger Derek; Parsons Ann; Tueller Jack
  Meeting abstracts of the Physical Society of Japan, Volume：58, Number：1, First page：91, Last page：91, 06 Mar. 2003
  The Physical Society of Japan (JPS), Japanese
  ISSN：1342-8349, CiNii Articles ID：110002212194, CiNii Books ID：AA11439205
• 28pSL-2 Astro-E2 衛星で狙う硬 X 線物理学　　　　　　　　　　　　　　　
  牧島 一夫; 国分 紀秀; 高橋 忠幸; 中澤 知洋; 深沢 泰司; 田代 信; 山岡 和貴; 寺田 幸功; 村上 敏夫; 米徳 大輔; 能町 正治; 釜江 常好; HXD team
  Volume：58, Number：1, First page：89, Last page：89, 06 Mar. 2003
  Japanese
  ISSN：1342-8349, CiNii Articles ID：110002212169, CiNii Books ID：AA11439205
• Swift Burst Alert Telescope Calibration (1)　　　　　　　　　　　　　　　
  Takahashi Hiromitsu; Okada Yuu; Kokubun Motohide; Makishima Kazuo; Sato Goro; Watanabe Shin; Nakazawa Kazuhiro; Takahashi Tadayuki; Suzuki Masaya; Tashiro Makoto; Barthelmy Scott; Cummings Jay; Krimm Hans; Gehrels Neil; Hullinger Derek; Parsons Ann; Tueller Jack
  Meeting abstracts of the Physical Society of Japan, Volume：58, Number：1, First page：90, Last page：90, 06 Mar. 2003
  The Physical Society of Japan (JPS), Japanese
  ISSN：1342-8349, CiNii Articles ID：110002212188, CiNii Books ID：AA11439205
• ガンマ線バースト観測衛星SwiftとBAT検出器　　　　　　　　　　　　　　　
  田代 信; 鈴木 雅也; 高橋 忠幸
  Volume：3, First page：281, Last page：284, 09 Jan. 2003
  Japanese
  CiNii Articles ID：80015960668, CiNii Books ID：AA11571712
• ガンマ線バースト観測衛星Swift搭載BAT検出器の有効面積の見積もり
  鈴木雅也; 田代信; 佐藤悟朗; 高橋忠幸; 中澤知洋; 渡辺伸; 岡田祐; 高橋弘充; BARTHELMY Scott; CUMMINGS Jay; GEHRELS Neil; HULLINGER Derek; KRIMM Hans; MARKWARDT Craig; PARSONS Ann; TULLER Jack; DEAN Tony; WIILIS Dave
  日本天文学会年会講演予稿集, Volume：2003, First page：242, 2003
  Japanese
  ISSN：1347-0639, J-Global ID：201302205818784517
• ガンマ線バースト観測用Swift衛星~Burst Alert Telescope~
  佐藤悟朗; 高橋忠幸; 中澤知洋; 渡辺伸; 鈴木雅也; 田代信; 岡田祐; 高橋弘充; BARTHELMY Scott; CUMMINGS Jay; GEHRELS Niel; HULLINGER Derek; KRIMM Hans; MARKWARDT Craig; PARSONS Ann; TULLER Jack
  日本天文学会年会講演予稿集, Volume：2003, First page：223, 2003
  Japanese
  ISSN：1347-0639, J-Global ID：201302272348123747
• ガンマ線バースト観測衛星Swift搭載BAT検出器の較正実験の評価
  鈴木雅也; 田代信; 高橋忠幸; 中澤知洋; 渡辺伸; 佐藤悟朗; 古宇田学; 牧島一夫; 国分紀秀; 岡田祐; 高橋弘充; GEHRELS N; PARSONS A; BARTHELMY S; TUELLER J; HULLINGER D; CUMMINGS J
  日本天文学会年会講演予稿集, Volume：2003, First page：224, 2003
  Japanese
  ISSN：1347-0639, J-Global ID：201302286431462414
• ガンマ線バースト観測用Swift衛星
  佐藤悟朗; 高橋忠幸; 中澤知洋; 渡辺伸; 鈴木雅也; 田代信; 岡田祐; 高橋弘充; BARTHELMY Scott; CUMMLNGS Jay; GEHRELS Neil; HULLINGER Derek; KRIMM Hans; MARKWARDT Craig; PARSONS Ann; TULLER Jack; DEAN Tony; WILLIS Dave
  日本天文学会年会講演予稿集, Volume：2003, First page：242, 2003
  Japanese
  ISSN：1347-0639, J-Global ID：201302287235741310
• 狭視野型軟γ線コンプトンカメラの感度の見積もり
  川埜直美; 阿部由紀子; 中本達也; 川添哲志; 深沢泰司; 三谷烈史; 中澤知洋; 高橋忠幸; 寺田幸功; 田代信; 国分紀秀; 牧島一夫
  日本天文学会年会講演予稿集, Volume：2003, First page：249, 2003
  Japanese
  ISSN：1347-0639, J-Global ID：201302251523318842
• Activation properties of Schottky CdTe diodes irradiated by 150 MeV protons　　　　　　　　　　　　　　　
  Mio M. Murakami; Yoshihito Kobayashi; Motohide Kokubun; Isao Takahashi; Yuu Okada; Madoka Kawaharada; Kazuhiro Nakazawa; Shin Walanabe; Goro Sato; Manabu Kouda; Takefumi Mitani; Tadayuki Takahashi; Masaya Suzuki; Makoto Tashiro; Kazuo Makishima
  IEEE Nuclear Science Symposium and Medical Imaging Conference, Volume：1, First page：269, Last page：273, 01 Dec. 2002
  With its high stopping power, Cadmium Telluride (CdTe) has been regarded as a promising semiconductor material for the next generation X/γ-ray detectors, and unproved significantly during this decade. In order to apply this device to astrophysics, it is essential to investigate the radiation hardness and background properties induced by cosmic-ray protons. We irradiated Scbottky CdTe diodes and a CdTe block with a beam of mono-energetic (150 MeV) protons. The induced radio-activation in CdTe was measured externally with a germanium detector, and internally with the irradiated CdTe diode itself. We successfully identified most of radioactive isotopes induced mainly via (p, xn) reactions, and confirmed that activation background level of the CdTe diode is sufficiently low in orbit. We compared energy resolution and leakage current before and after the irradiation, and also monitored the signals from a calibration source during the irradiation. There have been no significant degradation. CdTe diodes are enough tolerant to radioactivity in orbit.
  SCOPUS ID：0142241300
• A Chandra detection of diffuse hard X-ray emission associated with the lobes of the radio galaxy 3C 452　　　　　　　　　　　　　　　
  N Isobe; M Tashiro; K Makishima; N Iyomoto; M Suzuki; MM Murakami; M Mori; K Abe
  ASTROPHYSICAL JOURNAL, Volume：580, Number：2, First page：L111, Last page：L115, Dec. 2002
  An 80 ks Chandra ACIS observation of the radio galaxy 3C 452 is reported. A diffuse X-ray emission associated with the lobes has been detected with high statistical significance, together with the X-ray nucleus of the host galaxy. The 0.5-5 keV ACIS spectrum of the diffuse emission is described by a two-component model, consisting of a soft thermal plasma emission from the host galaxy halo and a hard nonthermal power-law component. The hard component is ascribed to the inverse Comptonization of cosmic microwave background photons by the synchrotron-emitting electrons in the lobes, because its spectral energy index, 0.68 +/- 0.28, is consistent with the radio synchrotron index, 0.78. These results reveal a significant electron dominance in the lobes. The electrons are inferred to have a relatively uniform distribution, while the magnetic field is compressed toward the lobe periphery.
  UNIV CHICAGO PRESS, English
  DOI：https://doi.org/10.1086/345658
  DOI ID：10.1086/345658, ISSN：0004-637X, Web of Science ID：WOS:000179458700005
• The apparent host galaxy of PKS 1413+135: Hubble Space Telescope, ASCA, and Very Long Baseline Array observations　　　　　　　　　　　　　　　
  ES Perlman; JT Stocke; CL Carilli; M Sugiho; M Tashiro; G Madejski; QD Wang; J Conway
  ASTRONOMICAL JOURNAL, Volume：124, Number：5, First page：2401, Last page：2412, Nov. 2002
  PKS 1413+135 (z=0.24671) is one of very few radio-loud active galactic nuclei (AGNs) with an apparent spiral host galaxy. Previous authors have attributed its nearly exponential infrared cutoff to heavy absorption but have been unable to place tight limits on the absorber or its location in the optical galaxy. In addition, doubts remain about the relationship of the AGN to the optical galaxy given the observed lack of reemitted radiation. We present new Hubble Space Telescope (HST), ASCA, and Very Long Baseline Array observations, which throw significant new light on these issues. The HST observations reveal that the active nucleus of PKS 1413+135 has an extremely red color, (V-H)=6.9 mag, requiring both a spectral turnover at a few microns because of synchrotron aging and an absorbing region the size of a giant molecular cloud. Combining constraints from the HST and ASCA data, we derive an intrinsic column NH=4.6(-1.6)(+2.1) x 10(22) cm(-2) and covering fraction f = 0.12(-0.05)(+0.07). The spin temperature of the molecular absorption lines found by previous authors suggests that the cloud is located in the disk of the optical galaxy, making our sight line rather unlikely (Psimilar to2x10(-4)). The properties of this region appear typical of large giant molecular clouds in our own Galaxy. The H I absorber appears centered 25 mas away from the nucleus, while the X-ray and nearly all of the molecular absorbers must cover the nucleus, implying a rather complicated geometry and cloud structure, in particular requiring a molecular core along our line of sight to the nucleus. Interestingly, the HST/NICMOS data require the AGN to be decentered relative to the optical galaxy by 13+/-4 mas. This could be interpreted as suggestive of an AGN location far in the background compared with the optical galaxy, but it can also be explained by obscuration and/or nuclear structure, which is more consistent with the observed lack of multiple images.
  IOP PUBLISHING LTD, English
  DOI：https://doi.org/10.1086/344109
  DOI ID：10.1086/344109, ISSN：0004-6256, Web of Science ID：WOS:000178768200003
• Development of Digital Electronics of Hard X-ray Detector on board Astro-E2(HXD2)　　　　　　　　　　　　　　　
  Terada Y.; Tashiro S.; Ezoe Y.; Takahashi H.; Suzuki M.; Mitani T.; Kokubun M.; Nakazawa K.; Yamaoka K.; Takahashi T.; Makishima K.; HXDteam
  Meeting abstracts of the Physical Society of Japan, Volume：57, Number：2, First page：80, Last page：80, 13 Aug. 2002
  The Physical Society of Japan (JPS), Japanese
  ISSN：1342-8349, CiNii Articles ID：110009718131, CiNii Books ID：AA11439205
• X-ray Probing into Energetics in Lobes of Radio Galaxies　　　　　　　　　　　　　　　
  Isobe Naoki; Makishima Kazuo; Tashiro Makoto; Suzuki Masaya; Murakami Mio; Abe Keiichi; Mori Masanori; Iyomoto Naoko
  Meeting abstracts of the Physical Society of Japan, Volume：57, Number：2, First page：75, Last page：75, 13 Aug. 2002
  The Physical Society of Japan (JPS), Japanese
  ISSN：1342-8349, CiNii Articles ID：110009718110, CiNii Books ID：AA11439205
• X-ray Observation of the radio galaxy 3C452 with Chandra　　　　　　　　　　　　　　　
  Mori M.; Isobe N.; Tasiro M.; Suzuki M.; Abe K.; Makishima K.; Fukazawa Y.; Iyomoto N.
  Meeting abstracts of the Physical Society of Japan, Volume：57, Number：2, First page：75, Last page：75, 13 Aug. 2002
  The Physical Society of Japan (JPS), Japanese
  ISSN：1342-8349, CiNii Articles ID：110009718109, CiNii Books ID：AA11439205
• The development and performance evaluation of the HXD-II onboard Astro-E2　　　　　　　　　　　　　　　
  Kawaharada M.; Ezoe Y.; Okada Y.; Kasama D.; Kokubun M.; Kotoku J.; Sugiho M.; Takahashi I.; Takahashi H.; Makishima K.; Miyawaki R.; Murakami M.; Yanagida T.; Ohno M.; Kawasoe T.; Kawano N.; Fukazawa Y.; Kobayashi Y.; Takahashi T.; Nakazawa K.; Mitani T.; Abe K; Tashiro M.; HXD members
  Meeting abstracts of the Physical Society of Japan, Volume：57, Number：2, First page：80, Last page：80, 13 Aug. 2002
  The Physical Society of Japan (JPS), Japanese
  ISSN：1342-8349, CiNii Articles ID：110009718130, CiNii Books ID：AA11439205
• SWift Burst Alert Telescope Calibration　　　　　　　　　　　　　　　
  Sato Goro; Okada Yuu; Watanabe Shin; Takahashi Tadayuki; Tashiro Makoto; Suzuki Masaya; Kouda Manabu; Sugiho Masahiko; Gehlres Neil; Tuller Jack; Scott Barthelmy; Parsons Ann; Hullinger Derek
  Meeting abstracts of the Physical Society of Japan, Volume：57, Number：2, First page：79, Last page：79, 13 Aug. 2002
  The Physical Society of Japan (JPS), Japanese
  ISSN：1342-8349, CiNii Articles ID：110009718126, CiNii Books ID：AA11439205
• Swift Mission and Gammna-rav Burst　　　　　　　　　　　　　　　
  Takahashi Tadayuki; Nakazawa Kazuhiro; Watanabe Shin; Sato Goro; Kouda Manabu; Ozawa Hideki; Tashiro Makoto; Suzuki Masaya; Okada Yu; Gehlres N.; Parsons A.; Scott B.; Tuller J.; Hullinger D.
  Meeting abstracts of the Physical Society of Japan, Volume：57, Number：2, First page：79, Last page：79, 13 Aug. 2002
  The Physical Society of Japan (JPS), Japanese
  ISSN：1342-8349, CiNii Articles ID：110009718125, CiNii Books ID：AA11439205
• Development of All-Sky-Monitor of Astro-E2HXD-II(2)　　　　　　　　　　　　　　　
  Hong S.; Yamaoka K.; Terada Y.; Kotoku J.; Mori M.; Tashiro M.; Fukazawa Y.; Kawasoe S.; Ohno M.; Takahashi T.; Kokubun M.; Makishima K.
  Meeting abstracts of the Physical Society of Japan, Volume：57, Number：2, First page：80, Last page：80, 13 Aug. 2002
  The Physical Society of Japan (JPS), Japanese
  ISSN：1342-8349, CiNii Articles ID：110009718129, CiNii Books ID：AA11439205
• Performance of the ASTRO-E hard X-ray detector　　　　　　　　　　　　　　　
  M Tashiro; T Kamae; K Makishima; T Takahashi; T Murakami; Y Fukazawa; M Kokubun; K Nakazawa; M Nomachi; A Yoshida; Y Ezoe; N Isobe; N Iyomoto; J Kataoka; J Kotoku; M Kouda; S Kubo; A Kubota; Y Matsumoto; T Mizuno; GM Madejski; Y Okada; N Ota; H Ozawa; G Sato; M Sugiho; M Sugizaki; Takahashi, I; H Takahashi; T Tamura; C Tanihata; Y Terada; Y Uchiyama; S Watanabe; K Yamaoka; D Yonetoku
  IEEE TRANSACTIONS ON NUCLEAR SCIENCE, Volume：49, Number：4, First page：1893, Last page：1897, Aug. 2002
  This paper summarizes the design and performance of the hard X-ray detector constructed for the ASTRO-E satellite. The detector utilizes the GSO/BGO well-type phoswich counters in a compound-eye configuration to achieve an extremely low background level of a few x 10(-5) counts s(-1) cm(-2)keV(-1) [1]. The GSO scintillators installed in the BGO active shield wells are sensitive to 30-600 keV photons, while the 2-mm-thick silicon PIN diodes, placed in front of each GSO crystal, cover the 10-60 keV energy band with a spectral resolution of similar to3.5-keV full-width at half-maximum. The design goals, of both low background and high energy resolution, in the hard X-ray bands were verified through the preflight calibration experiments.
  IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC, English
  DOI：https://doi.org/10.1109/TNS.2002.801491
  DOI ID：10.1109/TNS.2002.801491, ISSN：0018-9499, Web of Science ID：WOS:000178951100054
• 27aXD-3 XMM-Newton衛星による電波銀河Cantaurns Bの観測　　　　　　　　　　　　　　　
  鈴木 雅也; 田代 信; 磯部 直樹; 牧島 一夫; 深沢 泰司
  Volume：57, Number：1, First page：75, Last page：75, 01 Mar. 2002
  Japanese
  ISSN：1342-8349, CiNii Articles ID：110004063024, CiNii Books ID：AA11439205
• 26pZA-12 Proton beam experiment on new generation CdTe diode (2)　　　　　　　　　　　　　　　
  Kobayashi Y.; Murashima M.; Mitani T.; Kouda M.; Sato G.; Watanabe S.; Yonetoku D.; Nakazawa K.; Takahashi T.; Kawaharada M.; Okada Y.; Takahashi I.; Kokubun M.; Makishima K.; Suzuki M.; Tashiro M.
  Meeting abstracts of the Physical Society of Japan, Volume：57, Number：1, First page：161, Last page：161, 01 Mar. 2002
  The Physical Society of Japan (JPS), Japanese
  ISSN：1342-8349, CiNii Articles ID：110009770879, CiNii Books ID：AA11439205
• 26pZA-11 Protou beam experiment on new geueration CdTe diode (1)　　　　　　　　　　　　　　　
  murashima M; Kobayashi. Y.; Takahashi I.; Kokubum M.; kawaharada M.; Okada Y.; Nakazawa K.; Konda M.; Mitani T.; Sato G.; Watanabe S.; Yonetoku D.; Takahashi T; Suzuki. M.; Tashiro M.; Makishima K.
  Meeting abstracts of the Physical Society of Japan, Volume：57, Number：1, First page：161, Last page：161, 01 Mar. 2002
  The Physical Society of Japan (JPS), Japanese
  ISSN：1342-8349, CiNii Articles ID：110009770878, CiNii Books ID：AA11439205
• Astro-E2衛星硬X線検出器(HXD-11)のシールド部の開発　　　　　　　　　　　　　　　
  洪秀徴; 洪秀徴; 山岡和貴; 寺田幸功; 深沢泰司; 川添哲志; 大野雅功; 森正統; 田代信; 高橋忠幸; 古徳純一; 国分紀秀; 牧島一夫
  Volume：2002, 2002
  ISSN：1347-0639, J-Global ID：201402168858119006
• Variability timescales of TeV blazars observed in the ASCA continuous long-look X-ray monitoring　　　　　　　　　　　　　　　
  C Tanihata; CM Urry; T Takahashi; J Kataoka; SJ Wagner; GM Madejski; M Tashiro; M Kouda
  ASTROPHYSICAL JOURNAL, Volume：563, Number：2, First page：569, Last page：581, Dec. 2001
  Three uninterrupted, long (lasting respectively 7, 10, and 10 days) ASCA observations of the well-studied TeV-bright blazars Mrk 421, Mrk 501, and PKS 2155-304 all show continuous strong X-ray flaring. Despite the relatively faint intensity states in two of the three sources, there was no identifiable quiescent period in any of the observations. Structure function analysis shows that all blazars have a characteristic timescale of similar to1 day, comparable to the recurrence time and to the timescale of the stronger flares. On the other hand, examination of these flares in more detail reveals that each of the strong flares is not a smooth increase and decrease but exhibits substructures of shorter flares having timescales of similar to 10 ks. We verify via simulations that in order to explain the observed structure function, these shorter flares ("shots") are unlikely to be fully random, but in some way are correlated with each other. The energy dependent cross-correlation analysis shows that interband lags are not universal in TeV blazars. This is important since in the past only positive detections of lags were reported. In this work, we determine that the sign of a lag may differ from flare to flare; significant lags of both signs were detected from several flares, while no significant lag was detected from others. However, we also argue that the nature of the underlying component can affect these values. The facts that all flares are nearly symmetric and that fast variability shorter than the characteristic timescale is strongly suppressed, support the scenario where the light crossing time dominates the variability timescales of the day-scale flares.
  IOP PUBLISHING LTD, English
  DOI：https://doi.org/10.1086/323960
  DOI ID：10.1086/323960, ISSN：0004-637X, eISSN：1538-4357, Web of Science ID：WOS:000172852900011
• A possible X-ray periodicity at several tens of hours of an ultraluminous compact X-ray source in IC 342　　　　　　　　　　　　　　　
  M Sugiho; J Kotoku; K Makishima; A Kubota; T Mizuno; Y Fukazawa; M Tashiro
  ASTROPHYSICAL JOURNAL, Volume：561, Number：1, First page：L73, Last page：L76, Nov. 2001
  A long (155 hr) ASCA observation was performed of two ultraluminous compact X-ray sources, source 1 and source 2, in the spiral galaxy IC 342. While source 1, which was in a hard spectral state, varied little, source 2, which was in its soft spectral state, varied significantly on a timescale of about 1 day. The rms variation amplitude amounts to 5% in the 2-10 keV band but is less than 4% in 0.7- 2 keV. The variation involves statistically significant changes in the parameters describing multicolor disk blackbody emission from this source. The variation is possibly periodic, with a period of either 31 +/- 2 or 41 +/- 3 hr. Both are consistent with the orbital period of a semidetached binary formed by a black hole and a main-sequence star of several tens of solar masses. These results reinforce the interpretation of these X-ray objects in terms of accreting massive stellar black holes.
  UNIV CHICAGO PRESS, English
  DOI：https://doi.org/10.1086/324456
  DOI ID：10.1086/324456, ISSN：0004-637X, Web of Science ID：WOS:000171883700017
• A possible x-ray periodicity at several tens of hours of an ultraluminous compact x-ray source in IC 342　　　　　　　　　　　　　　　
  M. Sugiho; J. Kotoku; K. Makishima; A. Kubota; T. Mizuno; Y. Fukazawa; M. Tashiro
  Astrophysical Journal, Volume：561, Number：1, First page：L73, Last page：L76, 01 Nov. 2001
  A long (155 hr) ASCA observation was performed of two ultraluminous compact X-ray sources, source 1 and source 2, in the spiral galaxy IC 342. While source 1, which was in a hard spectral state, varied little, source 2, which was in its soft spectral state, varied significantly on a timescale of about 1 day. The rms variation amplitude amounts to 5% in the 2-10 keV band but is less than 4% in 0.7-2 keV. The variation involves statistically significant changes in the parameters describing multicolor disk blackbody emission from this source. The variation is possibly periodic, with a period of either 31 ± 2 or 41 ± 3 hr. Both are consistent with the orbital period of a semidetached binary formed by a black hole and a main-sequence star of several tens of solar masses. These results reinforce the interpretation of these X-ray objects in terms of accreting massive stellar black holes.
  Institute of Physics Publishing, English
  DOI：https://doi.org/10.1086/324456
  DOI ID：10.1086/324456, ISSN：1538-4357, SCOPUS ID：0035511190
• Status of BGO Anti-coincidence Counters of the Hard X-ray Detector onboard Astro-EII satellite　　　　　　　　　　　　　　　
  Yamaoka K.; Makishima K.; Kamae T.; Kokubun M.; Takahashi T.; Tashiro M.; Nakazawa K.; Murakami T.; Fukazawa Y.
  Meeting abstracts of the Physical Society of Japan, Volume：56, Number：2, First page：45, Last page：45, 03 Sep. 2001
  The Physical Society of Japan (JPS), Japanese
  ISSN：1342-8349, CiNii Articles ID：110002024424, CiNii Books ID：AA11439205
• Status report on the Hard X-ray Detector (HXD) aboard the ASTRO-E2 satellite (1)　　　　　　　　　　　　　　　
  Kokubun M.; Makishima K.; Takahashi T.; Murakami T.; Nakazawa K.; Tashiro S.; Fukazawa Y.; Kamae T.
  Meeting abstracts of the Physical Society of Japan, Volume：56, Number：2, First page：45, Last page：45, 03 Sep. 2001
  The Physical Society of Japan (JPS), Japanese
  ISSN：1342-8349, CiNii Articles ID：110002024423, CiNii Books ID：AA11439205
• Spatially dependent response of thick and large area p-i-n diode for ASTRO-E hard X-ray detector　　　　　　　　　　　　　　　
  M Sugiho; T Kamae; K Makishima; T Takahashi; T Murakami; M Tashiro; Y Fukazawa; N Iyomoto; H Ozawa; A Kubota; K Nakazawa; K Yamaoka; M Kokubun; N Ota; C Tanihata; N Isobe; Y Terada; Y Matsumoto; Y Uchiyama; D Yonetoku; Takahashi, I; J Kotoku; S Watanabe; Y Ezoe
  IEEE TRANSACTIONS ON NUCLEAR SCIENCE, Volume：48, Number：3, First page：426, Last page：429, Jun. 2001
  The ASTRO-E hard X-ray defector utilizes GSO(Gd2SiO5:Ce 0.5% mol)-BGO(Bi4Ge3O12) well-type phoswich counters [1] in compound-eye configuration to achieve an extremely low background level of about a few times 10(-5) counts s(-1) cm(-2) keV(-1). The GSO scintillators placed at the bottom of the BGO well observe photons in the energy range 30-600 keV. To cover the lower energy range of 10-60 keV, silicon p-i-n diodes of 2 mm in thickness and 21.5 x 21.5 mm(2) in size were newly developed and placed in front of the GSO scintillators. The p-i-n diode exhibits complex spectral responses, including subpeak and low energy tail components. To examine the origin of these components, we measured the spatially resolved response of the p-i-n diode and confirmed that the subpeak and the low energy tall are related to the electrode structures. and electric, fields in the p-i-n. diode, respectively.
  IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC, English
  DOI：https://doi.org/10.1109/23.940093
  DOI ID：10.1109/23.940093, ISSN：0018-9499, CiNii Articles ID：80012475086, Web of Science ID：WOS:000170576200038
• 28pSD-1 Astro-Eの再挑戦 : Astro-E-II衛星搭載用HXD-II検出器　　　　　　　　　　　　　　　
  高橋 忠幸; 牧島 一夫; 釜江 常好; 村上 敏夫; 田代 信; 深沢 泰司
  Volume：56, Number：1, First page：75, Last page：75, 09 Mar. 2001
  Japanese
  ISSN：1342-8349, CiNii Articles ID：110002155906, CiNii Books ID：AA11439205
• Discovery of spectral transitions from two ultraluminous compact X-ray sources in IC 342　　　　　　　　　　　　　　　
  A Kubota; T Mizuno; K Makishima; Y Fukazawa; J Kotoku; T Ohnishi; M Tashiro
  ASTROPHYSICAL JOURNAL, Volume：547, Number：2, First page：L119, Last page：L122, Feb. 2001
  Two ASCA observations were made of two ultraluminous compact X-ray sources (ULXs) in the spiral galaxy IC 342. In the 1993 observation, source 2 showed a 0.5-10 keV luminosity of 6 x 10(39) ergs s(-1) (assuming a distance of 4.0 Mpc) and a hard power-law spectrum of photon index similar to1.4. As already reported, source 1 was similar to3 times brighter on that occasion and exhibited a soft spectrum represented by a multicolor disk model with an inner- disk temperature of similar to 1.8 keV. The second observation, made in 2000 February, revealed that source 1 had made a transition into a hard spectral state, while source 2 made a transition into a soft spectral state. The ULXs are therefore inferred to exhibit two distinct spectral states, and they sometimes make transitions between them. These results significantly reinforce the scenario that describes ULXs as mass-accreting black holes.
  IOP PUBLISHING LTD, English
  DOI：https://doi.org/10.1086/318903
  DOI ID：10.1086/318903, ISSN：0004-637X, eISSN：1538-4357, Web of Science ID：WOS:000166732800008
• ASCA observations of the BL Lacertae object OJ 287 in 1997 April and November　　　　　　　　　　　　　　　
  N Isobe; M Tashiro; M Sugiho; K Makishima
  PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN, Volume：53, Number：1, First page：79, Last page：83, Feb. 2001
  The X-ray properties of the BL Lacertae object OJ 287, observed with ASCA on 1997 April 26 and November 17, are reported. The 0.5-10 keV flux was lower than that obtained in previous X-ray observations, and no evidence of intensity variations was found during each observation. The obtained flux densities at 1 keV, 0.22-0.26 mu Jy, exceed the extrapolations from lower frequency synchrotron continua, which were measured in nearly the same period as the present ASCA observations. The X-ray spectra acquired with the GIS and SIS were consistently described with a single power-law model modified by the Galactic absorption, and the derived photon indices, 1.5-1.6, are flatter than those observed so far. These results strongly suggest that the X-ray spectra observed in 1997 arise via an inverse Compton process alone. The X-ray spectra obtained in 1994 (Idesawa et al. 1997, AAA 68.159.334), exhibiting a steeper slope than those in 1997, is thought to be contaminated by a "synchrotron soft tail".
  OXFORD UNIV PRESS, English
  DOI：https://doi.org/10.1093/pasj/53.1.79
  DOI ID：10.1093/pasj/53.1.79, ISSN：0004-6264, eISSN：2053-051X, Web of Science ID：WOS:000167293400010
• ASTRO‐E2衛星に搭載される硬X線検出器(HXD‐II)の現状
  中澤知洋; 牧島一夫; 高橋忠幸; 村上敏夫; 田代信; 深沢泰司; 国分紀秀; 能町正治; 釜江常好
  日本天文学会年会講演予稿集, Volume：2001, First page：307, 2001
  Japanese
  ISSN：1347-0639, J-Global ID：201402128764344373
• X-ray measurements of the field and particle energy distributions in the west lobe of the radio galaxy NGC 1316 (Fornax A)　　　　　　　　　　　　　　　
  M Tashiro; K Makishima; N Iyomoto; N Isobe; H Kaneda
  ASTROPHYSICAL JOURNAL, Volume：546, Number：1, First page：L19, Last page：L23, Jan. 2001
  A follow-up X-ray study was made of the west lobe of the radio galaxy Fornax A (NGC 1316) that was based on new ASCA observations made in 1997 for 98 ks and that incorporated the previous observation in 1994 for 39 ks. The 0.7-10 keV spectrum of the emission can be described by a power law with an energy index of 0.74 +/- 0.10 which agrees with the synchrotron radio index of 0.9 +/- 0.2. Therefore, the X-rays are reconfirmed to arise via the inverse Compton scattering of the cosmic microwave photons, as Kaneda et al. and Feigelson et al. concluded. The surface brightness of the inverse Compton X-rays exhibits a relatively flat distribution over the west lobe, indicative of an approximately spherical emissivity distribution with a radius of similar to 11 ' (75 kpc). In contrast, the 1.4 GHz radio image by Ekers et al. exhibits a rim-brightened surface brightness, consistent with a shell-like emissivity distribution whose inner and outer boundaries are 4 ' and 11 ', respectively. These morphological differences between radio and X-rays suggest that the relativistic electrons are distributed homogeneously over the lobe volume, whereas the magnetic field is amplified toward the lobe rim region.
  IOP PUBLISHING LTD, English
  DOI：https://doi.org/10.1086/318057
  DOI ID：10.1086/318057, ISSN：0004-637X, eISSN：1538-4357, Web of Science ID：WOS:000166457000005
• ASCA and other contemporaneous observations of the blazar B2 1308+326　　　　　　　　　　　　　　　
  D Watson; N Smith; L Hanlon; B McBreen; F Quilligan; M Tashiro; L Metcalfe; P Doyle; H Terasranta; A Carraminana; J Guichard
  ASTRONOMY & ASTROPHYSICS, Volume：364, Number：1, First page：43, Last page：52, Dec. 2000
  The high redshift (z = 0.997) blazar B2 1308+326 was observed contemporaneously at x-ray, optical and radio wavelengths in June 1996. The x-ray observations were performed with ASCA. The ASCA results were found to be consistent with reanalysed data from two earlier ROSAT observations. The combined ASCA and ROSAT data reveal an xray spectrum that is best fit by a broken power law with absorber model with photon spectral indices of Gamma (soft) = 3.4(-1.1)(+5.1) and Gamma (hard) = 1.63(-0.09)(+0.10) and a break energy at 1.1(-0.4)(+0.4) keV in the rest-frame of the blazar. The break in the x-ray spectrum is interpreted, from the shape of the simultaneous broadband spectral energy distribution, to be the emerging importance of inverse Compton (IC) emission which dominates the ASCA spectrum. The faint optical state reported for these observations (m(V) = 18.3 +/- 0.25) is incompatible with the high synchrotron flux previously detected by ROSAT. The TC emission detected by both ROSAT and ASCA was not significantly affected by the large change in the synchrotron component.
  Mg II emission was detected with an equivalent width (W-lambda) of similar to 15 Angstrom, significantly different from previously reported values. The small and variable W-lambda in B2 1308+326 may be due to the highly variable continuum and not intrinsically weak lines in the source. A lower limit on the Doppler boost factor calculated from the contemporaneous data is consistent with expectations for highly polarised quasars and higher than expected for BL Lacs. Absorption at a level of N-H = 3.0(-0.6)(+2.3) x 10(20) cm(-2) was detected which is in excess of the Galactic value of NH 1.1 x 10(20) cm(-2), indicating the possible presence of a foreground absorber. A gravitational microlensing scenario cannot therefore be ruled out for this blazar. No significant variability on timescales of hours was detected in the optical or x-ray data.
  B2 1308+326 could be a typical radio-selected BL Lac in terms of peak synchrotron frequency and optical and radio variability but its high bolometric luminosity, variable line emission and high Doppler boost factor make it appear more like a quasar than a BL Lac. It is suggested that B2 1308+326 be considered as the prototype of this class of composite source.
  EDP SCIENCES S A, English
  ISSN：1432-0746, Web of Science ID：WOS:000166412300016
• Complex spectral variability from intensive multiwavelength monitoring of Markarian 421 in 1998　　　　　　　　　　　　　　　
  T Takahashi; J Kataoka; G Madejski; J Mattox; CM Urry; S Wagner; F Aharonian; M Catanese; L Chiappetti; P Coppi; B Degrange; G Fossati; H Kubo; H Krawczynski; F Makino; H Marshall; L Maraschi; F Piron; R Remillard; F Takahara; M Tashiro; H Terasranta; T Weekes
  ASTROPHYSICAL JOURNAL, Volume：542, Number：2, First page：L105, Last page：L109, Oct. 2000
  We conducted a multifrequency campaign for the TeV blazar Markarian 421 in 1998 April. The campaign started from a pronounced high-amplitude flare recorded by BeppoSAX and Whipple; the ASCA observation started 3 days later. In the X-ray data, we detected multiple flares, occurring on timescales of about 1 day. ASCA data clearly reveal spectral variability. The comparison of the data from ASCA, the Extreme Ultraviolet Explorer, and the Rossi X-Ray Timing Explorer indicates that the variability amplitudes in the low-energy synchrotron component are larger at higher photon energies. In TeV gamma -rays, large intraday variations-which were correlated with the X-ray flux-were observed when results from three Cerenkov telescopes were combined. The rms variability of TeV gamma -rays was similar to that observed in hard X-rays, above 10 keV. The X-ray light curve reveals flares that are almost symmetric for most cases, implying that the dominant timescale is the light crossing time through the emitting region. The structure function analysis based on the continuous X-ray light curve of 7 days indicates that the characteristic timescale is similar to0.5 days. The analysis of ASCA light curves in various energy bands appears to show both soft (positive) and hard (negative) lags. These may not be real, as systematic effects could also produce these lags, which are all much smaller than an orbit. If the lags of both signs are red, these imply that the particle acceleration and X-ray cooling timescales are similar.
  IOP PUBLISHING LTD, English
  DOI：https://doi.org/10.1086/312929
  DOI ID：10.1086/312929, ISSN：0004-637X, eISSN：1538-4357, Web of Science ID：WOS:000165095700008
• Development of new hard X-gamma ray detector with GSO scintillator and photodiode　　　　　　　　　　　　　　　
  Takahashi I.; Oonishi T.; Makishima K.; Tashiro S.; Kamae T.
  Meeting abstracts of the Physical Society of Japan, Volume：55, Number：2, First page：49, Last page：49, 10 Sep. 2000
  The Physical Society of Japan (JPS), Japanese
  ISSN：1342-8349, CiNii Articles ID：110002186758, CiNii Books ID：AA11439205
• Measurements of field-electron energy distributions in radio lobes　　　　　　　　　　　　　　　
  Tashiro M.; Makishima K.; Isobe N.; Kaneda H.
  Meeting abstracts of the Physical Society of Japan, Volume：55, Number：2, First page：66, Last page：66, 10 Sep. 2000
  The Physical Society of Japan (JPS), Japanese
  ISSN：1342-8349, CiNii Articles ID：110002187073, CiNii Books ID：AA11439205
• Energy response of PIN diode developed for ASTRO-E Hard X-ray Detector　　　　　　　　　　　　　　　
  Sugiho M.; Kamae T.; Makihsima K.; Tashiro M.; Fukazawa Y.; Takahashi T.; Murakami T.; Ohta N; Yonetoku D; Watanabe S
  Meeting abstracts of the Physical Society of Japan, Volume：55, Number：2, First page：67, Last page：67, 10 Sep. 2000
  The Physical Society of Japan (JPS), Japanese
  ISSN：1342-8349, CiNii Articles ID：110002187088, CiNii Books ID：AA11439205
• ASCA Dicoveries of X-ray Emissions from Radio Lobes　　　　　　　　　　　　　　　
  TASHIRO Makoto
  The Astronomical herald, Volume：93, Number：9, First page：487, Last page：495, 20 Aug. 2000
  Japanese
  ISSN：0374-2466, CiNii Articles ID：10004583746, CiNii Books ID：AN00154555
• The nature of ultraluminous compact X-ray sources in nearby spiral galaxies　　　　　　　　　　　　　　　
  K Makishima; A Kubota; T Mizuno; T Ohnishi; M Tashiro; Y Aruga; K Asai; T Dotani; K Mitsuda; Y Ueda; S Uno; K Yamaoka; K Ebisawa; Y Kohmura; K Okada
  ASTROPHYSICAL JOURNAL, Volume：535, Number：2, First page：632, Last page：643, Jun. 2000
  Studies were made of ASCA spectra of seven ultraluminous compact X-ray sources in nearby spiral galaxies: M33 X-8, M81 X-6, IC 342 source 1, Dwingeloo 1 X-1, NGC 1313 source B, and two sources in NGC 4565. With the 0.5-10 keV luminosities in the range 10(39)-10(40) ergs s(-1), they are thought to represent a class of enigmatic X-ray sources often found in spiral galaxies. For some of them, the ASCA data are newly processed or the published spectra are reanalyzed. For others, the published results are quoted. The ASCA spectra of all seven sources have been described successfully with so-called multicolor disk blackbody emission arising from optically thick standard accretion disks around black holes. Except for the case of M33 X-8, the spectra do not exhibit hard tails. For the source luminosities not to exceed the Eddington limits, the black holes are inferred to have rather high masses, up to similar to 100 M.. However, the observed innermost disk temperatures of these objects, T-in = 1.1-1.8 keV, are too high to be compatible with the required high black hole masses, as long as the standard accretion disks around Schwarzschild black holes are assumed. Similarly high disk temperatures are also observed from two Galactic transients with superluminal motions, GRO 1655-40 and GRS 1915 + 105. The issue of unusually high disk temperature may be explained by the black hole rotation, which makes the disk get closer to the black hole and hence hotter.
  IOP PUBLISHING LTD, English
  DOI：https://doi.org/10.1086/308868
  DOI ID：10.1086/308868, ISSN：0004-637X, eISSN：1538-4357, Web of Science ID：WOS:000087789500012
• ASTRO‐E衛星 硬X線検出器HXD有効面積の角度応答
  松本縁; 中澤知洋; 深沢泰司; 田代信; 釜江常好; 牧島一夫; 高橋忠幸; 村上敏夫
  日本天文学会年会講演予稿集, Volume：2000, First page：179, 2000
  Japanese
  ISSN：1347-0639, J-Global ID：201402130884189902
• ASTRO‐E衛星搭載用硬X線検出器(HXD)の地上最終キャリブレーション(2)
  杉保昌彦; 釜江常好; 牧島一夫; 田代信; 深沢泰司; 国分紀秀; 中澤知洋; 磯部直樹; 松本縁; 江副祐一郎; 高橋勲; 高橋忠幸; 村上敏夫; 太田直美; 谷畑千春; 内山泰伸; 米徳大輔; 渡辺伸
  日本天文学会年会講演予稿集, Volume：2000, First page：178, 2000
  Japanese
  ISSN：1347-0639, J-Global ID：201402185986716205
• Variability pattern and the spectral evolution of the BL lacertae object PKS 2155-304　　　　　　　　　　　　　　　
  J Kataoka; T Takahashi; F Makino; S Inoue; GM Madejski; M Tashiro; CM Urry; H Kubo
  ASTROPHYSICAL JOURNAL, Volume：528, Number：1, First page：243, Last page：253, Jan. 2000
  The TeV blazar PKS 2155 - 304 was monitored with the X-ray satellite ASCA in 1994 May as part of a multiwavelength campaign from the radio to X-ray bands. At the beginning of the two-day continuous observation, we detected a lame flare, in which the 2-10 keV flux changed by a factor of 2 on a timescale of 3 x 10(4) s. During the hare, the increase in the hard X-ray flux clearly preceded that observed in the soft X-rays, with the spectral evolution tracking a "clockwise loop" in the flux versus photon index plane. Ascribing the energy-dependent variability to differential synchrotron cooling of relativistic electrons, we estimate the magnetic field B in the emission region. We tested two different methods of comparing the time series in various X-ray bands: (1) fitting the light curves to a Gaussian function and searching for the time shift of the peak of the flare, and (2) calculating the discrete correlation function. Both methods yielded a consistent solution of B similar to 0.1 G; We also found that the flare amplitude becomes larger as the photon energy increases, while the duration of the flare stays roughly constant throughout the ASCA energy band (0.7-7.5 keV). In the framework of the time-dependent synchrotron self-Compton model in a homogeneous region, we consider a flare where the maximum Lorentz factor (gamma(max)) of the injected electrons increases uniformly throughout the emission volume. The temporal evolution of spectra as well as the light curves were reproduced with the physical parameters self-consistently determined from seven observables. We obtained B similar to 0.1-0.2 G and a region size R similar to 10(-2) pc for relativistic beaming with a Doppler factor of delta similar to 20-30. We discuss the significance of light-travel time effects.
  UNIV CHICAGO PRESS, English
  DOI：https://doi.org/10.1086/308154
  DOI ID：10.1086/308154, ISSN：0004-637X, Web of Science ID：WOS:000084941100021
• ASCA observations of blazars and multiband analysis　　　　　　　　　　　　　　　
  H Kubo; T Takahashi; G Madejski; M Tashiro; F Makino; S Inoue; F Takahara
  BROAD BAND X-RAY SPECTRA OF COSMIC SOURCES, Volume：25, Number：3-4, First page：733, Last page：736, 2000
  We present data for 18 blazars observed with ASCA, half of which were also observed contemporaneously with EGRET as parts of multi-wavelength campaigns. The ASCA X-ray spectra of High-energy peaked BL Lacs (HBLs) are soft, and they form the highest energy tail of the low energy (synchrotron) component. The X-ray spectra of the quasar-hosted blazars (QHBs) are hard and consistent with the lowest energy end of the high energy (Compton) component. For Low-energy peaked BL Lacs (LBLs), the X-ray spectra are intermediate. We find that the radiation process responsible for the HE peak for HBLs can be explained solely by Synchrotron-Self-Compton (SSC) emission. For many QHBs, on the other hand, the gamma-rays cannot be solely due to the SSC mechanism. We consider an alternative scenario for QHBs where the SSC component dominates in the X-ray band, but it is below the observed gamma-ray spectrum. We infer the magnetic field B to be 0.1 - 1 Gauss, and Lorentz factors gamma(b) of electrons radiating at the peak of the nu F(nu) spectrum of similar to 10(3) for QHBs. This is much lower than gamma(b) similar to 10(5) for HBLs. (C) 2000 COSPAR. Published by Elsevier Science Ltd.
  PERGAMON PRESS LTD, English
  DOI：https://doi.org/10.1016/S0273-1177(99)00831-5
  DOI ID：10.1016/S0273-1177(99)00831-5, ISSN：0273-1177, Web of Science ID：WOS:000085367000074
• ASCA measurements of field-particle energy distribution in radio lobes　　　　　　　　　　　　　　　
  M Tashiro; K Makishima; H Kaneda
  BROAD BAND X-RAY SPECTRA OF COSMIC SOURCES, Volume：25, Number：3-4, First page：751, Last page：756, 2000
  The ASCA detections of inverse-Compton (IC) X-rays from lobes of radio galaxies are reported. Significant IC X-rays are observed from radio lobes of Fornax A (Kaneda et al. 1995; Feigelson et al. 1995), Centaurus B (PKS 1343-601) and NGC 612. The energy density and magnetic field intensity in the lobes are sorted out by comparing the IC X-ray flux with the synchrotron radio flux. The results from Centaurus B strongly suggest particle domination in the lobes; meanwhile, X-ray and radio image analysis shows an outward increase in the magnetic energy density. The X-ray image and spectrum observed from NGC: 612 reveal a heavily absorbed low luminosity core (nucleus) emission, together with an extended emission associated with the lobes. The extended source luminosity is rather close to the expected value assuming the equipartition state, although the possibility of particle dominant lobes cannot be excluded. (C) 2000 COSPAR. Published by Elsevier Science Ltd.
  PERGAMON PRESS LTD, Romanian, Moldavian, Moldovan
  DOI：https://doi.org/10.1016/S0273-1177(99)00834-0
  DOI ID：10.1016/S0273-1177(99)00834-0, ISSN：0273-1177, Web of Science ID：WOS:000085367000077
• ASCA observations of two ultra-luminous compact X-ray sources in the edge-on spiral galaxy NGC 4565　　　　　　　　　　　　　　　
  T Mizuno; T Ohnishi; A Kubota; K Makishima; M Tashiro
  PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN, Volume：51, Number：5, First page：663, Last page：671, Oct. 1999
  The edge-on spiral galaxy NGC 4565 was observed for similar to 35 ks with ASCA in the 0.5-10 keV energy band. The X-ray emission was dominated by two bright sources, which could be identified with two point-like X-ray sources seen in the ROSAT HRI image. The observed 0.5-10 keV fluxes of these sources, 1.7 x 10(-12) erg s(-1) cm(-2) and 0.7 x 10(-12) erg s(-1) cm(-2), imply bolometric luminosities of 1.2 x 10(40) erg s(-1) and 4.6 x 10(39) erg s(-1), respectively. They exhibit similar spectra, which can be explained by emission from optically thick accretion disks with inner-disk temperature of 1.4-1.6 keV. One of them, coincident in position with the nucleus, shows too low absorption to be the active nucleus seen through the galaxy disk. Their spectra and high luminosities suggest that they are both mass-accreting black-hole binaries. However, the black-hole mass required by the Eddington limit is rather high (greater than or equal to 50M.), and the observed disk temperature is too high to be compatible with the high black-hole mass. Several attempts have been made to solve these problems.
  OXFORD UNIV PRESS, English
  DOI：https://doi.org/10.1093/pasj/51.5.663
  DOI ID：10.1093/pasj/51.5.663, ISSN：0004-6264, eISSN：2053-051X, Web of Science ID：WOS:000083375300011
• 25pSD-9 Astro-E搭載硬X線検出器の地上特性評価試験　　　　　　　　　　　　　　　
  谷畑 千春; 高橋 忠幸; 片岡 淳; 田代 信; 深沢 泰司; 牧島 一夫; 釜江 常好; HXDチーム
  Volume：54, Number：2, First page：82, Last page：82, 13 Sep. 1999
  Japanese
  ISSN：1342-8349, CiNii Articles ID：110002059093, CiNii Books ID：AA11439205
• 25pSD-8 Development and Performance of PIN diodes for the ASTRO-E HXD　　　　　　　　　　　　　　　
  OTA N; MURAKAMI T; TAKAHASHI T; TAMURA T; MAKISHIMA K; KAMAE T; TASHIRO M; FUKAZAWA Y; HXD Team
  Meeting abstracts of the Physical Society of Japan, Volume：54, Number：2, First page：82, Last page：82, 13 Sep. 1999
  The Physical Society of Japan (JPS), Japanese
  ISSN：1342-8349, CiNii Articles ID：110002059091, CiNii Books ID：AA11439205
• 25pSD-10 The Preflight Calibration of the ASTRO-E Hard X-ray Detector(HXD)　　　　　　　　　　　　　　　
  ISOBE N; KAMAE T; MAKISHIMA K; MURAKAMI T; TAKAHASHI T; TASHIRO M; FUKAZAWA Y; SUGIHO M; UCHIYAMA Y; MATSUMOTO Y; NAKAZAWA K; KOKUBUN M; TAKAHASHI I; HXD Team
  Meeting abstracts of the Physical Society of Japan, Volume：54, Number：2, First page：82, Last page：82, 13 Sep. 1999
  The Physical Society of Japan (JPS), Japanese
  ISSN：1342-8349, CiNii Articles ID：110002059095, CiNii Books ID：AA11439205
• Simultaneous multifrequency observations of the BL Lac MS 0205.7+3509　　　　　　　　　　　　　　　
  D Watson; L Hanlon; B McBreen; N Smith; M Tashiro; AR Foley; L Metcalfe; Beckmann, V; SF Sanchez; H Terasranta
  ASTRONOMY & ASTROPHYSICS, Volume：345, Number：2, First page：414, Last page：418, May 1999
  Radio and optical observations of the possible microlensed BL Lac source MS 0205.7+3509 were obtained simultaneously with ASCA x-ray measurements in February 1997. A single power law model, with a photon index of 2.61, is an adequate fit to the ASCA data, once hydrogenic absorption in excess of the Galactic value is permitted, confirming a previous ROSAT measurement. On the basis of our simultaneous data we have determined MS 0205.7+3509 to be a typical x-ray selected BL Lac, with alpha(xox) = -0.82. There is no indication of an inverse Compton (IC) component in the ASCA spectrum up to 10 keV. No evidence for variability on hour-long timescales is present in either the x-ray or the optical data. We discuss these results in the context of a gravitational microlensing scenario for MS 0205.7+3509.
  EDP SCIENCES S A, English
  ISSN：0004-6361, Web of Science ID：WOS:000080300300011
• 25pSD-2 X-ray Observations of ultra-luminous X-ray sources in neaby spiral galaxies with ASCA　　　　　　　　　　　　　　　
  MIZUNO T; MAKISHIMA K; TASHIRO M; KUBOTA A; OHNISHI T; KOTOKU J
  Meeting Abstracts of the Physical Society of Japan, Volume：54, Number：0, First page：80, Last page：80, 1999
  一般社団法人 日本物理学会, Japanese
  ISSN：1342-8349, CiNii Articles ID：110002059081, CiNii Books ID：AA11439205
• ASCA Observations of Two Ultra-Luminous Compact X-Ray Sources in the Edge-On Spiral Galaxy NGC 4565　　　　　　　　　　　　　　　
  Mizuno, T; Ohnishi, T; Kubota, A; Makishima, K; Tashiro, M
  Publications of the Astronomical Society of Japan, Volume：51, First page：663, Last page：671, 1999
• Activation of the ASTRO-E hard X-ray detector in low earth orbit　　　　　　　　　　　　　　　
  M. Kokubun; Y. Fukazawa; E. Idesawa; J. Kataoka; T. Kamae; K. Matsuzaki; T. Mizuno; Y. Saito; T. Takahashi; K. Takizawa; M. Tashiro; T. Tamura; A. Yoshida
  IEEE Transactions on Nuclear Science, Volume：46, Number：3, First page：371, Last page：376, 1999
  ASTRO-E Hard X-ray Detector (HXD) is characterized by well-type phoswich counters[1] in a compound-eye configuration which reduce the detector background to lower level than any other past hard X-ray mission. When operating in Low Earth Orbit, the expected background of the HXD is an order of 10 -5 counts/s/kcV/cm 2, mainly caused from the radioactivity induced within the detector materials by geomagnetically trapped protons. Results are presented from measurements of induced radioactivity in two phoswich scintillators, GSO (Gd 2SiO 5:Ce 0.5% mol) and BGO (Bi 4Ge 3O 12), irradiated by mono-energetic protons at an accelerator facility. Radiation transport computer codes are used to build the detector response functions for emissions from decays of spallation products. Based on the comparison between experimental and simulation results, the activation background level of HXD in the orbit is estimated. © 1999 IEEE.
  English
  DOI：https://doi.org/10.1109/23.775546
  Scopus：https://www.scopus.com/inward/record.uri?partnerID=HzOxMe3b&scp=0033339792&origin=inward
  Scopus Citedby：https://www.scopus.com/inward/citedby.uri?partnerID=HzOxMe3b&scp=0033339792&origin=inward
  DOI ID：10.1109/23.775546, ISSN：0018-9499, CiNii Articles ID：80011257138, SCOPUS ID：0033339792
• 4a-E-8 「あすか」による低光度AGN M81の時間変動の研究II　　　　　　　　　　　　　　　
  伊予本 直子; 牧島 一夫; 田代 信; 久保田 あや; 石碕 欣尚; 林田 清
  Volume：53, Number：2, First page：84, Last page：84, 05 Sep. 1998
  Japanese
  ISSN：1342-8349, CiNii Articles ID：110001988597, CiNii Books ID：AA11439205
• Observasion of BL Lacertac Object OJ287 with ASCA　　　　　　　　　　　　　　　
  SUGIHO Masahiko; ISOBE Naoki; TASHIRO Makoto; MAKISHIMA Kazuo
  Meeting abstracts of the Physical Society of Japan, Volume：53, Number：2, First page：84, Last page：84, 05 Sep. 1998
  The Physical Society of Japan (JPS), Japanese
  ISSN：1342-8349, CiNii Articles ID：110001988598, CiNii Books ID：AA11439205
• Measurement of the Response of the ASTRO-E Hare X-ray Detecto　　　　　　　　　　　　　　　
  ISOBE N.; TERADA Y.; MATSUMOTO Y.; TANIHATA T.; MAKISHIMA K.; KAMAE T.; TAKAHASHI T.; TASHIRO M.; FUKAZAWA Y.; KOKUBUN M.; YAMAOKA K.; NAKAZAWA K.; HXD TEAM
  Meeting abstracts of the Physical Society of Japan, Volume：53, Number：2, First page：82, Last page：82, 05 Sep. 1998
  The Physical Society of Japan (JPS), Japanese
  ISSN：1342-8349, CiNii Articles ID：110001988592, CiNii Books ID：AA11439205
• ASCA observations of blazars and multiband analysis　　　　　　　　　　　　　　　
  H Kubo; T Takahashi; G Madejski; M Tashiro; F Makino; S Inoue; F Takahara
  ASTROPHYSICAL JOURNAL, Volume：504, Number：2, First page：693, Last page：701, Sep. 1998
  We present data for 18 blazars observed with the X-ray satellite ASCA, half of which were also observed contemporaneously with the EGRET instrument onboard Compton Gamma Ray Observatory as parts of multiwavelength campaigns. The observations show a clear difference in the spectra between three subclasses of blazars, namely, high-energy peaked BL Lacertae objects (HBLs), low-energy peaked BL Lac objects (LBLs), and quasar-hosted blazars (QHBs). The ASCA X-ray spectra of HBLs are the softest, with the power-law energy index alpha similar to 1-2, and they form the highest observable energy tail of the low-energy (LE, synchrotron) component. The X-ray spectra of the QHBs are the hardest (alpha similar to 0.6) and are consistent with the lowest observable energy end of the high-energy (HE, Compton) component. For LBLs, the X-ray spectra are intermediate. We find that the radiation process responsible for the HE peak for HBLs can be explained solely by Doppler-boosted synchrotron self-Compton (SSC) emission, with the Doppler factor delta consistent with the VLBI and/or gamma-ray variability data. For many QHBs, on the other hand, the gamma-rays cannot be solely a result of the SSC mechanism unless delta is significantly in excess of that inferred from VLBI data. We consider an alternative scenario consistent with the measured values of delta, where the SSC component is still present in QHBs and dominates in the X-ray band but is below the observed gamma-ray spectrum. With an assumption that the peak of the SSC emission is on the extrapolation of the X-ray spectrum, and adopting a value of 10 for delta, we infer the magnetic field B to be 0.1-1 G and Lorentz factors gamma(b) of electrons radiating at the peak of the nu F(nu) spectrum of similar to 10(3) for QHBs; this is much lower than gamma(b) similar to 10(5) for HBLs, even though the Values of B are comparable in the two subclasses. This difference of gamma(b) is most likely due to the large photon density expected in QHBs (e.g., from thermal components visible in these objects) as compared with that of HBLs; Compton upscattering of these photons may well provide the observed GeV flux.
  IOP PUBLISHING LTD, English, Book review
  DOI：https://doi.org/10.1086/306125
  DOI ID：10.1086/306125, ISSN：0004-637X, eISSN：1538-4357, Web of Science ID：WOS:000077777500010
• Low-luminosity X-ray active galactic nuclei in S0 galaxies NGC 3065 and NGC 4203　　　　　　　　　　　　　　　
  N Iyomoto; K Makishima; K Matsushita; Y Fukazawa; M Tashiro; T Ohashi
  ASTROPHYSICAL JOURNAL, Volume：503, Number：1, First page：168, Last page：173, Aug. 1998
  We present ASCA X-ray results on two SO galaxies, NGC 3065 and NGC 4203. In both galaxies, we detected hard X-ray emission from a pointlike source at the nucleus. A single power-law model having a photon index of similar to 1.8 well described the spectra of these sources, while thin thermal emission, which is common in SO galaxies, was not detected. The 2-10 keV luminosities of these nuclear sources (2.2 x 10(41) and 1.5 x 10(40) ergs s(-1)) are 1-2 orders of magnitude higher than those expected as an assembly of low-mass X-ray binaries in these galaxies. Our results strongly suggest that NGC 3065 and NGC 4203 host low-luminosity active galactic nuclei.
  IOP PUBLISHING LTD, English
  DOI：https://doi.org/10.1086/305974
  DOI ID：10.1086/305974, ISSN：0004-637X, eISSN：1538-4357, Web of Science ID：WOS:000077776400014
• The declined activity in the nucleus of NGC 1316　　　　　　　　　　　　　　　
  N Iyomoto; K Makishima; M Tashiro; S Inoue; H Kaneda; Y Matsumoto; T Mizuno
  ASTROPHYSICAL JOURNAL, Volume：503, Number：1, First page：L31, Last page：L34, Aug. 1998
  NGC 1316 (Fornax A) is a radio galaxy with prototypical double lobes, when the magnetic field intensity is accurately measured via the inverse Compton technique. The radio-emitting electrons in the lobes are inferred to have a synchrotron lifetime of similar to 0.1 Gyr. Considering the lobe energetics, we estimate the past nuclear X-ray luminosity of NGC 1316 to be at least similar to 4 x 10(34) W (4 X 10(41) ergs s(-1)). Thus, the nucleus was rather active at least 0.1 Gyr ago. In contrast, we confirmed with ASCA and ROSAT that the nucleus of NGC 1316 is very faint in X-rays at present, with the 2-10 keV luminosity of any active galactic nucleus-like hard component being less than 2 x 10(33) W (2 x 10(40) ergs s(-1)), even assuming a nuclear obscuration up to similar to 10(28) m(-2) (10(24) cm(-2)). This is at least an order of magnitude lower than the estimated past activity, indicating that the nucleus is presently very inactive. From these two results, we conclude that the nucleus of NGC 1316 has become dormant during the last 0.1 Gyr. This suggests the possible abundance of "dormant" quasars in nearby galaxies.
  UNIV CHICAGO PRESS, English
  DOI：https://doi.org/10.1086/311518
  DOI ID：10.1086/311518, ISSN：0004-637X, Web of Science ID：WOS:000077776500008
• Evidence of energy nonequipartition between particles and fields in lobes of the radio galaxy PKS 1343-601 (Centaurus B)　　　　　　　　　　　　　　　
  M Tashiro; H Kaneda; K Makishima; N Iyomoto; E Idesawa; Y Ishisaki; T Kotani; T Takahashi; A Yamashita
  ASTROPHYSICAL JOURNAL, Volume：499, Number：2, First page：713, Last page：718, Jun. 1998
  We observed the radio galaxy PKS 1343-601 (Centaurus B) in X-rays with ASCA and discovered diffuse hard X-ray emission from its radio lobe region. The obtained flux and spectrum strongly suggest that the X-rays are produced via an inverse-Compton (IC) process, in which the cosmic microwave background photons are boosted up to X-rays by synchrotron electrons. This is the second case, following the case of Fornax A, of the detection of the IC X-rays from radio lobes. The observed X-ray emission is brighter than expected in the case of minimum energy density, indicating particle-dominated lobes, Comparison of the X-ray and radio images reveals an outward increase in the magnetic energy density. This infers a gradual compression of magnetic fields toward the edge of the lobes.
  UNIV CHICAGO PRESS, English
  DOI：https://doi.org/10.1086/305655
  DOI ID：10.1086/305655, ISSN：0004-637X, Web of Science ID：WOS:000074172200016
• ASCA observations of a nearby and massive galaxy cluster Abell 3627　　　　　　　　　　　　　　　
  T Tamura; Y Fukazawa; H Kaneda; K Makishima; M Tashiro; Y Tanaka; H Bohringer
  PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN, Volume：50, Number：2, First page：195, Last page：201, Apr. 1998
  The results obtained from ASCA observations of the cluster of galaxies Abell 3627 are presented. This cluster, located behind the Milky Way, was recently found to be a nearby, X-ray bright, and very rich cluster. Pointed observations onto the central region of the cluster gave a gas temperature of similar to 7 keV and a metallicity of about 0.2 solar. An offset pointing to a substructure elongated to the south-east of the cluster center gave a significantly lower temperature of similar to 5 keV. The 2-10 keV luminosity within a radius of 40' (1.1 Mpc) is estimated to be 3.7 x 10(44) erg s(-1). The X-ray data imply a cluster mass of about 4 x 10(14) M-. within 40'.
  OXFORD UNIV PRESS, English
  DOI：https://doi.org/10.1093/pasj/50.2.195
  DOI ID：10.1093/pasj/50.2.195, ISSN：0004-6264, eISSN：2053-051X, Web of Science ID：WOS:000073317400001
• X-ray Observations of the normal spiral galaxies with ASCA　　　　　　　　　　　　　　　
  MIZUNO T.; TASHIRO M.; MAKISHIMA K.; MATSUSHITA K.
  Meeting abstracts of the Physical Society of Japan, Volume：53, Number：1, First page：81, Last page：81, 10 Mar. 1998
  The Physical Society of Japan (JPS), Japanese
  ISSN：1342-8349, CiNii Articles ID：110002174290, CiNii Books ID：AA11439205
• 2a-J-5 ASTRO-E搭載硬X線検出器アナログ処理回路の開発(phoswich-I)　　　　　　　　　　　　　　　
  谷畑 千春; 片岡 淳; 寺田 幸功; 水野 恒史; 江澤 元; 田代 信; 深沢 泰司; 高橋 忠幸; 牧島 一夫; 釜江 常好; 森國 城
  Volume：53, Number：1, First page：80, Last page：80, 10 Mar. 1998
  Japanese
  ISSN：1342-8349, CiNii Articles ID：110002174268, CiNii Books ID：AA11439205
• Surface coating of the ASTRO-E PIN detector and its long-term performance　　　　　　　　　　　　　　　
  OTA N.; MURAKAMI T.; OSAWA H.; KUBO S.; SUGIZAKI M.; TAKAHASHI T.; MITSUDA K.; MAKISHIMA K.; KAMAE T.; TASHIRO M.; FUKASAWA Y.
  Meeting abstracts of the Physical Society of Japan, Volume：53, Number：1, First page：79, Last page：79, 10 Mar. 1998
  The Physical Society of Japan (JPS), Japanese
  ISSN：1342-8349, CiNii Articles ID：110002174252, CiNii Books ID：AA11439205
• X-ray observations of the BL Lac object PKS0548-322 with ASCA　　　　　　　　　　　　　　　
  TASHIRO M.; MAKISHIMA K.; ISOBE N.; KOTANI T.; YAMASHITA A.; HAYASHIDA K.
  Meeting abstracts of the Physical Society of Japan, Volume：53, Number：1, First page：83, Last page：83, 10 Mar. 1998
  The Physical Society of Japan (JPS), Japanese
  ISSN：1342-8349, CiNii Articles ID：110002174325, CiNii Books ID：AA11439205
• 2p-J-2 「あすか」による低光度AGNの時間変動の研究　　　　　　　　　　　　　　　
  伊予本 直子; 牧島 一夫; 田代 信; 石崎 欣尚; 林田 清; 久保田 あや
  Volume：53, Number：1, First page：83, Last page：83, 10 Mar. 1998
  Japanese
  ISSN：1342-8349, CiNii Articles ID：110002174330, CiNii Books ID：AA11439205
• Monte Carlo evaluation of the ASTRO-E Hard X-ray Detector　　　　　　　　　　　　　　　
  KOKUBUN M; FUKAZAWA Y; MAKISHIMA K; MATSUZAKI K; MATSUMOTO Y; YAMAOKA K; HXD TEAM; ISOBE N; KAMAE T; KUBOTA A; TAKAHASHI T; TANIHATA C; TASHIRO M; TERADA Y; NAKAZAWA K
  Meeting Abstracts of the Physical Society of Japan, Volume：53, Number：0, First page：82, Last page：82, 1998
  一般社団法人 日本物理学会, Japanese
  ISSN：1342-8349, CiNii Articles ID：110001988591, CiNii Books ID：AA11439205
• X-ray observations of the BL Lacertae object OJ 287 with ASCA　　　　　　　　　　　　　　　
  E Idesawa; M Tashiro; K Makishima; K Kubo; C Otani; T Ohashi
  PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN, Volume：49, Number：6, First page：631, Last page：637, Dec. 1997
  Reports have been made on the X-ray properties of the BL Lacertae object OJ 287, obtained with ASCA on 1994 November 18-19. Although the observation was made during a period of enhanced optical intensity, the obtained 0.5-10 keV flux falls below those from previous X-ray observations. Intensity variations on time scales of a few hours were detected, with a typical peak-to-peak amplitude of 20%. The X-ray spectra acquired with the SIS and the GIS are described consistently with a single power-law model with the galactic absorption, and the required photon index, similar to 1.7, is flatter than most of those previously observed from this object. The derived monochromatic X-ray flux at 1 keV, 0.76 mu Jy, exceeds the extrapolation from the lower frequency continua, which is based on near-simultaneous multi-band observations. A discussion is made concerning the origin of X-ray emission from OJ 287 in terms of the synchrotron and synchrotron-self-Compton mechanisms.
  OXFORD UNIV PRESS, English
  DOI：https://doi.org/10.1093/pasj/49.6.631
  DOI ID：10.1093/pasj/49.6.631, ISSN：0004-6264, eISSN：2053-051X, Web of Science ID：WOS:000071179900002
• 23a-J-12 Evidence for a dramatic activity decline in the nucleus of the radio galaxy　　　　　　　　　　　　　　　
  Iyomoto N.; Makishima K.; Kaneda H.; Tashiro M.; Fukazawa Y.; Osone S.
  Meeting abstracts of the Physical Society of Japan, Volume：52, Number：2, First page：80, Last page：80, 02 Sep. 1997
  The Physical Society of Japan (JPS), Japanese
  ISSN：1342-8349, CiNii Articles ID：110001981290, CiNii Books ID：AA11439205
• 23a-J-11 X-ray observations of the Radio Galaxy NGC612 with ASCA　　　　　　　　　　　　　　　
  Tashiro M.; Makishima K.; Kaneda H.; Inoue H.; Sugizaki M.
  Meeting abstracts of the Physical Society of Japan, Volume：52, Number：2, First page：79, Last page：79, 02 Sep. 1997
  The Physical Society of Japan (JPS), Japanese
  ISSN：1342-8349, CiNii Articles ID：110001981289, CiNii Books ID：AA11439205
• 23p-J-3 Hierarchical Distributions of the Dark Matter discovered with ASCA　　　　　　　　　　　　　　　
  Makishima K; Ikebe Y; Xu H; Matsushita K; Fukazawa Y; Ohashi T; Tashiro M; Tamura T
  Meeting abstracts of the Physical Society of Japan, Volume：52, Number：2, First page：81, Last page：81, 02 Sep. 1997
  The Physical Society of Japan (JPS), Japanese
  ISSN：1342-8349, CiNii Articles ID：110001981297, CiNii Books ID：AA11439205
• Multiwavelength monitoring of the BL Lacertae object PKS 2155-304 in 1994 May .3. Probing the inner jet through multiwavelength correlations　　　　　　　　　　　　　　　
  CM Urry; A Treves; L Maraschi; HL Marshall; T Kii; G Madejski; S Penton; JE Pesce; E Pian; A Celotti; R Fujimoto; F Makino; C Otani; RM Sambruna; K Sasaki; JM Shull; PS Smith; T Takahashi; M Tashiro
  ASTROPHYSICAL JOURNAL, Volume：486, Number：2, First page：799, Last page：809, Sep. 1997
  In 1994 May, the BL Lac object PKS 2155-304 was observed continuously for similar to 10 days with the International Ultraviolet Explorer and the Extreme Ultraviolet Explorer and for 2 days with ASCA, as well as with ROSAT and with ground-based radio, infrared, and optical telescopes. The light curves show a well-defined X-ray flare followed by a broader, lower amplitude extreme-ultraviolet flare similar to 1 day later and a broad, low-amplitude UV flare similar to 2 days later. X-ray fluxes obtained at three well-separated times the preceding week indicate at least one previous flare of comparable amplitude or perhaps ongoing stochastic X-ray variations, and additional rapid variability was seen at the beginning of the IUE observation, when extremely sharp changes in UV flux occurred. The X-ray flux observed with ASCA flared by a factor of similar to 2 in about half a day and decayed roughly as fast. In contrast, the subsequent UV flare had an amplitude of only similar to 35% and lasted longer than 2 days.
  Assuming that the X-ray, EUV, and UV events are associated, the lags, the decrease of amplitude with wavelength, and the broadening of the temporal profile with wavelength are all qualitatively as expected for synchrotron emission from an inhomogeneous, relativistic jet. Because of the high quality of the data, we can rule out that the observed flares were caused by either a Fermi-type shock acceleration event or a pair cascade in a homogeneous synchrotron-emitting region. A homogeneous region is still possible if there was an instantaneous (t much less than hours) injection of high-energy electrons that emit first at X-ray energies. Alternatively, the data are consistent with a compression wave or other disturbance crossing a region with stratified particle energy distributions. This kind of situation is expected to occur behind a shock front and/or in an inhomogeneous jet. The present light curves are in sharp contrast to the multiwavelength variability observed in 1991 November, when the amplitude was wavelength independent and the UV lagged the X-rays by less than similar to 3 hr. This means that the origin of rapid multiwavelength variability in this blazar is complex, involving at least two different modes.
  UNIV CHICAGO PRESS, English
  DOI：https://doi.org/10.1086/304536
  DOI ID：10.1086/304536, ISSN：0004-637X, Web of Science ID：WOS:A1997XX17300016
• Evidence of an ionized iron emission line from the radio-quiet quasar E1821+643 by ASCA　　　　　　　　　　　　　　　
  A Yamashita; C Matsumoto; M Ishida; H Inoue; T Kii; K Makishima; T Takahashi; M Tashiro
  ASTROPHYSICAL JOURNAL, Volume：486, Number：2, First page：763, Last page：769, Sep. 1997
  We present the results of an ASCA observation of the radio-quiet quasar E1821 + 643. The 2-10 keV flux and the power-law index are consistent with the values reported previously by EXOSAT, Ginga, and BBXRT. The iron K-emission line feature discovered by the Ginga observations is confirmed, and its redshift-corrected, line-center energy is better determined to be 6.58 +/- 0.05 keV. This line feature shows marginal broadening with an upper limit of 180 eV in Gaussian sigma (in the quasar rest frame). The line equivalent width is 170 +/- 50 eV in the quasar rest frame, which is consistent with the Ginga measurement, and the contribution from the quasar-associated cluster of galaxies is estimated to be negligible.
  IOP PUBLISHING LTD, English
  DOI：https://doi.org/10.1086/304554
  DOI ID：10.1086/304554, ISSN：0004-637X, Web of Science ID：WOS:A1997XX17300013
• Detection of strong Fe-K lines from the spiral galaxies NGC 1365 and NGC 1386　　　　　　　　　　　　　　　
  N Iyomoto; K Makishima; Y Fukazawa; M Tashiro; Y Ishisaki
  PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN, Volume：49, Number：4, First page：425, Last page：434, Aug. 1997
  Two spiral galaxies, NGC 1365 and NGC 1386, were observed in X-rays with ASCA. Both galaxies exhibit hard X-ray emission from point-like sources at the nuclei. The continuous spectrum of NGC 1365 was fitted well with a power-law of photon index 0.8(-0.2)(+0.7), whose 2-10 keV luminosity is (3.8+/-0.5) x 10(40) erg s(-1) for an assumed distance of 18.4 Mpc. NGC 1386 has an absorbed [N-H=(2.8(-2.6)(+2.7)) x 10(23) cm(-2)] power-law continuum, whose 2-10 keV luminosity (at 18.4 Mpc) is (2.6(-2.0)(+3.2)) x 10(40) erg s(-1) after removing the absorption. A broad (sigma=0.20(-0.08)(+0.16) keV) Fe-K emission line centered at 6.61(-0.06)(+0.08) keV was detected from the NGC 1365 nucleus at an equivalent width of 2.1(-0.3)(+2.1) keV. The Fe-K line was also detected from NGC 1386 at an equivalent width of 1.6(-1.2)(+7.9) keV and at a similar energy as the NGC 1365 line. These spectral features indicate that both galaxies host low-luminosity active galactic nuclei (LLAGNs).
  OXFORD UNIV PRESS, English
  DOI：https://doi.org/10.1093/pasj/49.4.425
  DOI ID：10.1093/pasj/49.4.425, ISSN：0004-6264, eISSN：2053-051X, Web of Science ID：WOS:A1997XV62300004
• 30p-YM-8 Activation of GSO, BGO scintillators for Hard X-ray Detectors　　　　　　　　　　　　　　　
  Kokubun M.; Idesawa E.; Kataoka J.; Kamae T.; Saito Y.; Takahashi T.; Takizawa K.; Tashiro M.; Fukazawa Y.; Makishima K.; Matsuzaki K.; Mizuno T.; Yoshida A.; HXD team
  Meeting abstracts of the Physical Society of Japan, Volume：52, Number：1, First page：74, Last page：74, 17 Mar. 1997
  The Physical Society of Japan (JPS), Japanese
  ISSN：1342-8349, CiNii Articles ID：110002172380, CiNii Books ID：AA11439205
• 30p-YM-7 Activation of HXD onboard the Astro-E satellite　　　　　　　　　　　　　　　
  Takizawa K.; Idesawa E.; Kataoka J.; Kamae T.; Kokubun M.; Saito Y.; Takahashi T.; Tashiro M.; Fukazawa Y.; Makishima K.; Matsuzaki K.; Mizuno T.; Yoshida A.; HXD team
  Meeting abstracts of the Physical Society of Japan, Volume：52, Number：1, First page：74, Last page：74, 17 Mar. 1997
  The Physical Society of Japan (JPS), Japanese
  ISSN：1342-8349, CiNii Articles ID：110002172375, CiNii Books ID：AA11439205
• 28a-YY-3 Structure Development Hard of X-ray Detector (HXD) for Astro-E Satellite　　　　　　　　　　　　　　　
  Nakazawa K.; Iyomoto N.; Obayasi H.; Kaneda H.; Matsuzaki K.; Saito Y.; Isobe N.; Kamae T.; Makishima K.; Fukazawa Y.; Tashiro M.; Murakami T.; HXD-team
  Meeting abstracts of the Physical Society of Japan, Volume：52, Number：1, First page：82, Last page：82, 17 Mar. 1997
  The Physical Society of Japan (JPS), Japanese
  ISSN：1342-8349, CiNii Articles ID：110002172475, CiNii Books ID：AA11439205
• Development of the hard X-ray detector for the ASTRO-E mission　　　　　　　　　　　　　　　
  T Takahashi; H Ezawa; Y Fukazawa; M Hirayama; E Idesawa; H Ikeda; Y Ishisaki; N Iyomoto; T Kamae; J Kataoka; H Kaneda; H Kubo; K Makishima; K Matsushita; K Matsuzaki; T Mizuno; T Murakami; K Nagata; S Nakamae; M Nomachi; H Obayashi; T Ohtsuka; H Ozawa; Y Saito; M Sugizaki; T Tamura; M Tashiro; N Tsuchida; K Tsukada; A Yoshida
  ASTRONOMY & ASTROPHYSICS SUPPLEMENT SERIES, Volume：120, Number：4, First page：C645, Last page：C648, Dec. 1996
  The Hard X-ray Detector (HXD) is one of three instruments on the fifth Japanese X-ray astronomy satellite, ASTRO-E, scheduled for launch in 2000. The HXD consists of a 4x4 = 16 modular assembly of identical counters, each consisting of a combination of YAP(or GSO)/BGO well-type phoswich counters and silicon PIN diodes. The field of view of the detector for high energy photons is restricted to 4 degrees x 4 degrees by active collimators made of BGO and the fov for low energy photons is restricted to 0.5 degrees x 0.5 degrees by the fine passive collimators made of phosphor bronze. The detector is characterized by a low background reaching severalx10(-6) c/s/cm(2)/keV. Combined with the other two instruments for soft X-ray observations (0.5-12 keV), the ASTRO-E mission will cover the entire range of soft and hard X-rays with the highest sensitivity ever achieved. Furthermore, thick EGO counters which surround the 4x4 matrix of well-type phoswich counters act as a gamma-ray burst detector in the energy band of 100-2000 keV.
  EDITIONS PHYSIQUE, English
  ISSN：0365-0138, Web of Science ID：WOS:A1996WC06300145
• ASCA observation of an X-ray/TeV flare from the BL Lacertae object Markarian 421　　　　　　　　　　　　　　　
  T Takahashi; M Tashiro; G Madejski; H Kubo; T Kamae; J Kataoka; T Kii; F Makino; K Makishima; N Yamasaki
  ASTROPHYSICAL JOURNAL, Volume：470, Number：2, First page：L89, Last page：L92, Oct. 1996
  We observed the BL Lac object Mrk 421 with the X-ray satellite ASCA in 1994 as part of a multifrequency observation. The 24 hr observation was conducted 1 day after the onset of a TeV flare detected by the Whipple Observatory and detected an X-ray flare, with no apparent variability in the optical, UV, and EGRET GeV flux. The ASCA 2-10 keV flux peaked at 3.7 x 10(-10) ergs cm(-2) s(-1) and then decreased to 1.8 x 10(-10) ergs cm(-2) s(-1) with a doubling timescale of similar to 12 hr. The shape of the X-ray spectrum varied during the observation, such that the hard X-rays always led the soft X-rays, both in brightening and dimming of the source, with a lag of the 0.5-1 keV photons versus those in the 2-7.5 keV band of similar to 1 hr. The rapid TeV variability indicates a compact TeV-producing region, suggesting relativistic beaming with a Doppler factor delta greater than or equal to 5. The correlation of the flux in the X-ray and the TeV bands indicates that a high-energy tail of a single electron population is responsible for both X-rays and TeV gamma-rays, with radio, IR, UV and X-rays produced via the synchrotron process and GeV and TeV gamma-rays produced via Comptonization. Under the assumption that the ''soft lag'' observed in the X-ray band is due to the synchrotron-lifetime effects, with delta = 5, we calculate the magnetic field for the X-ray-producing region to be similar to 0.2 G. The Lorentz factors gamma(el) of the electrons responsible for the emission in the keV and TeV bands are similar to 10(6), consistent with the values implied by the Klein-Nishina limit.
  UNIV CHICAGO PRESS, English
  DOI：https://doi.org/10.1086/310302
  DOI ID：10.1086/310302, ISSN：0004-637X, Web of Science ID：WOS:A1996VM99900004
• ASCA observations of the composite warm absorber in NGC 3516　　　　　　　　　　　　　　　
  GA Kriss; JH Krolik; C Otani; BR Espey; TJ Turner; T Kii; Z Tsvetanov; T Takahashi; AF Davldsen; M Tashiro; W Zheng; S Murakami; R Petre; T Mihara
  ASTROPHYSICAL JOURNAL, Volume：467, Number：2, First page：629, Last page：635, Aug. 1996
  We obtained X-ray spectra of the Seyfert 1 galaxy NGC 3516 in 1995 March using the Japanese X-ray satellite, ASCA. Simultaneous far-UV observations were obtained with the Hopkins Ultraviolet Telescope on the Astro-2 shuttle mission. The ASCA spectrum shows a lightly absorbed power law of energy index 0.78. The low-energy absorbing column is significantly less than previously seen. Prominent O VII and O VIII absorption edges are visible, but, consistent with the much lower total absorbing column, no Fe K absorption edge is detectable. A weak, narrow Fe K alpha emission line from cold material is present as well as a broad Fe K alpha line. These features are similar to those reported in other Seyfert 1 galaxies. A single warm absorber model provides only an imperfect description of the low-energy absorption. In addition to a highly ionized absorber with ionization parameter U = 1.66 and a total column density of 1.4 x 10(22) cm(-2), adding a lower ionization absorber with U = 0.32 and a total column of 6.9 x 10(21) cm(-2) significantly improves the fit. The contribution of resonant line scattering to our warm absorber models limits the Doppler parameter to less than 160 km s(-1) at 90% confidence. Turbulence at the sound speed of the photoionized gas provides the best fit. None of the warm absorber models fitted to the X-ray spectrum can match the observed equivalent widths of all the UV absorption lines. Accounting for the X-ray and UV absorption simultaneously requires an absorbing region with a broad range of ionization parameters and column densities.
  UNIV CHICAGO PRESS, English
  DOI：https://doi.org/10.1086/177638
  DOI ID：10.1086/177638, ISSN：0004-637X, Web of Science ID：WOS:A1996VD21800015
• An ASCA observation of the x-ray binary GX 301-2　　　　　　　　　　　　　　　
  P Saraswat; A Yoshida; T Mihara; N Kawai; T Takeshima; F Nagase; K Makishima; M Tashiro; DA Leahy; S Pravdo; CSR Day; L Angelini
  ASTROPHYSICAL JOURNAL, Volume：463, Number：2, First page：726, Last page：736, Jun. 1996
  The X-ray binary pulsar GX 301-2 was observed with the Advanced Satellite for Cosmology and Astrophysics (ASCA) on 1994 February 13-14, at the binary orbital phase between 0.277 and 0.308. The source was found to be in a low-intensity phase, with an intrinsic luminosity L(X) = 6.6 x 10(35) ergs s(-1) in the 0.7-10.0 keV energy band. This is roughly 2 orders of magnitude lower than the peak luminosity generally observed at periastron. The spectral analysis shows the presence of a strong low-energy excess below about 4 keV and high photoelectric absorption (similar to 6 x 10(23) cm(-2)). Part of the soft excess may be caused by the scattering of X-rays around a region of increased density by the less dense ambient stellar wind, which would explain the absence of pulsations in the low-energy excess. The spectrum also shows a strong, narrow fluorescent iron line and an absorption iron K edge. The average energy of the line is 6.400 +/- 0.008 keV and that of the edge is 7.183 +/- 0.013 keV (at the 90% confidence level). The iron line equivalent width is 228 +/- 18 eV. The partial covering model does not describe the low-energy excess adequately. It underestimates the continuum between 2.0 and 5.0 keV but overestimates it below 1.5 keV. This, together with the absence of pulsations in the low-energy excess, rules out the partial covering model as a good description of the continuum spectrum.
  In addition, the spectra from the solid-state imaging spectrometers (SIS) aboard ASCA reveal two new features. First, it is seen that the fit with the scattering model is not acceptable below 2 keV and suggests an additional component as cause for this residual soft excess. The ultrasoft component has been observed in the spectra of GX 301-2 for the first time and can be fitted well by thermal emission from a hot plasma with a temperature kT of similar to 0.8 keV. The ultrasoft component may arise because of emission from X-ray-induced shocks in the gas trailing the neutron star. A partial ionization model with a warm absorber in series with a neutral absorber, including scattering, does not account for the ultrasoft excess below 1.5 keV and can be ruled out. Second, it is also seen that the SIS spectrum is dominated by line features at 0.80, 1.73, 2.30, 2.98, and 3.68 keV. These can be identified with the fluorescent line emission from neutral or near-neutral Ne, Si, S, Ar, and Ca, respectively. This implies that the line emission is coming from cold (less than or equal to 10(5) K) gas.
  The pulse phase spectroscopy shows that the photon index, the iron line intensity, and the equivalent width vary with pulse phase. The large equivalent width variations are, however, mainly due to the changes in the underlying continuum intensity.
  UNIV CHICAGO PRESS, English
  DOI：https://doi.org/10.1086/177285
  DOI ID：10.1086/177285, ISSN：0004-637X, Web of Science ID：WOS:A1996UM94500031
• The gas imaging spectrometer on board ASCA　　　　　　　　　　　　　　　
  T Ohashi; K Ebisawa; Y Fukazawa; K Hiyoshi; M Horii; Y Ikebe; H Ikeda; H Inoue; M Ishida; Y Ishisaki; T Ishizuka; S Kamijo; H Kaneda; Y Kohmura; K Makishima; T Mihara; M Tashiro; T Murakami; R Shoumura; Y Tanaka; Y Ueda; K Taguchi; T Tsuru; T Takeshima
  PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN, Volume：48, Number：2, First page：157, Last page：170, Apr. 1996
  The Gas Imaging Spectrometer (GIS) system on board ASCA is described. The experiment consists of 2 units of imaging gas scintillation proportional counters with a sealed-off gas cell equipped with an imaging phototube. The performance is characterized by the high X-ray sensitivity (from 0.7 keV to over 10 keV), good energy resolution (7.8% FWHM at 6 keV following E(-0.5) as a function of X-ray energy E), moderate position resolution (0.5 mm FWHM at 6 keV with E(-0.5) dependence), fast time resolution down to 61 mu s, and an effective area of 50 mm diameter. The on-board signal processing system and the data transmitted to the ground are also described. The background rejection efficiency of the GIS is reaching the level achieved by the non-imaging multi-cell proportional counters.
  OXFORD UNIV PRESS, English
  DOI：https://doi.org/10.1093/pasj/48.2.157
  DOI ID：10.1093/pasj/48.2.157, ISSN：0004-6264, eISSN：2053-051X, Web of Science ID：WOS:A1996UJ29200003
• In-orbit performance of the gas imaging spectrometer onboard ASCA　　　　　　　　　　　　　　　
  K Makishima; M Tashiro; K Ebisawa; H Ezawa; Y Fukazawa; S Gunji; M Hirayama; E Idesawa; Y Ikebe; M Ishida; Y Ishisaki; N Iyomoto; T Kamae; H Kaneda; K Kikuchi; Y Kohmura; H Kubo; K Matsushita; K Matsuzaki; T Mihara; K Nakagawa; T Ohashi; Y Saito; Y Sekimoto; T Takahashi; T Tamura; T Tsuru; Y Ueda; NY Yamasaki
  PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN, Volume：48, Number：2, First page：171, Last page：189, Apr. 1996
  The in-orbit performance and calibration of the Gas Imaging Spectrometer (GIS), located on the focal plane of the X-ray astronomy satellite ASCA, are described. An extensive in-orbit calibration has confirmed its basic performance, including a position resolution of 0.6 mm (FWHM) and an energy resolution of 7.8% (FWHM), both at 6 keV. When combined with the X-ray telescope, the GIS sensitivity range becomes 0.7-10 keV. The in-orbit non X-ray background of the GIS has been confirmed to be as low as (5-9) x 10(-4) cs(-1) cm(-2) keV(-1) over the 1-10 keV range. The long-term detector gain has been stable within a few ro for nearly 3 years. Extensive observations of the Crab Nebula and other sources have provided accurate calibrations of the position response, photometric capability, dead time, and timing accuracy of the GIS. Furthermore, the overall energy response, including the temporal and positional gain variations and the absolute gain scale, has been calibrated to similar to 1%. Thus, the GIS is working as an all-round cosmic X-ray detector, capable of X-ray imagery, fine X-ray spectroscopy, X-ray photometry With a flux dynamic range covering more than 5 orders of magnitude, and fast X-ray photometry with a time resolution up to 60 mu s.
  OXFORD UNIV PRESS, English
  DOI：https://doi.org/10.1093/pasj/48.2.171
  DOI ID：10.1093/pasj/48.2.171, ISSN：0004-6264, eISSN：2053-051X, Web of Science ID：WOS:A1996UJ29200004
• Detection of excess hard X-ray emission from the optical jet galaxy NGC 1097　　　　　　　　　　　　　　　
  N Iyomoto; K Makishima; Y Fukazawa; M Tashiro; Y Ishisaki; N Nakai; Y Taniguchi
  PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN, Volume：48, Number：2, First page：231, Last page：236, Apr. 1996
  Using the ASCA observatory, X-ray observations were made of the spiral galaxy NGC 1097, which exhibits four optical jets. Hard X-ray emission from a point-like source at the nucleus was detected at a 2-10 keV luminosity of 1 x 10(41) erg s(-1) for an assumed distance of 24 Mpc. The 2-10 keV spectrum was well fitted with a power-law of photon index similar to 1.8. Although no X-ray variability was detected during a similar to 40 ks pointing, the observed X-ray to optical luminosity ratio of NGC 1097 is too. high for the X-ray emission to be explained by an assembly of discrete X-ray sources. From our results and optical activity, the existence of a low-luminosity active galactic nucleus (LLAGN) is strongly suggested. In the soft X-ray band (0.5-2 keV) a thin thermal emission with a temperature kT similar to 0.6 keV was also detected, which is understood to be emission from hot gas associated with starburst activity.
  OXFORD UNIV PRESS, English
  DOI：https://doi.org/10.1093/pasj/48.2.231
  DOI ID：10.1093/pasj/48.2.231, ISSN：0004-6264, eISSN：2053-051X, Web of Science ID：WOS:A1996UJ29200009
• Simultaneous soft X-ray and GeV gamma-ray observations of BL Lacertae object AO 0235+164　　　　　　　　　　　　　　　
  G Madejski; T Takahashi; M Tashiro; H Kubo; R Hartman; T Kallman; M Sikora
  ASTROPHYSICAL JOURNAL, Volume：459, Number：1, First page：156, Last page：168, Mar. 1996
  We present data collected during a simultaneous GeV gamma-ray (Compton Gamma Ray Observatory EGRET) and X-ray (ASCA) observation of BL Lac object AO 0235+164 (z = 0.94); we also present ROSAT PSPC X-ray data, obtained 6 months earlier. The X-ray spectra from both ROSAT and ASCA confirm a substantial photoelectric absorption beyond the value expected from our Galaxy, which is most likely caused by heavy elements in the inerstellar medium of an intervening galaxy at z = 0.524; it is possible to measure the elemental abundances in it module the hydrogen spin temperature T-S. By comparing the absorption in our data to the 21 cm absorption, we can limit TS to at most similar to 700 K.
  The ROSAT data imply a rapid (similar to 3 day) doubling of the soft X-ray flux and a subsequent quasi-exponential decay, whereas no variability is apparent in the ASCA or EGRET data. We detect a significant spectral change of the BL Lac X-ray continuum between the ROSAT and ASCA observations; ASCA data show that the spectrum is substantially harder (with the energy power-law index alpha similar to 1 vs. similar to 2) and fainter than in the ROSAT data. The simplest interpretation of this spectral variability is that the ROSAT data are dominated by a bright, soft tail of a synchrotron component, which disappeared during the ASCA observation, uncovering a harder Compton component.
  The EGRET data imply a lower GeV flux than in the previous observations, with no apparent change of the GeV spectrum. The ratio of the gamma-ray to the X-ray flux [in E x F(E)] for this radio-discovered object is roughly 30, which is very substantially higher than that inferred for X-ray-discovered BL Lac objects, suggesting an important difference in the structure between the two subclasses of BL Lac objects.
  UNIV CHICAGO PRESS, English
  DOI：https://doi.org/10.1086/176877
  DOI ID：10.1086/176877, ISSN：0004-637X, Web of Science ID：WOS:A1996TV79100014
• Multiwavelength observations of Markarian 421 during a TeV/X-ray flare (vol 449, pg L99, 1995)　　　　　　　　　　　　　　　
  DJ Macomb; CW Akerlof; HD Aller; MF Aller; DL Bertsch; F Bruhweiler; JH Buckley; DA CarterLewis; MF Cawley; KP Cheng; C Dermer; DJ Fegan; JA Gaidos; WK Gear; CR Hall; RC Hartman; AM Hillas; M Kafatos; AD Kerrick; DA Kniffen; Y Kondo; H Kubo; RC Lamb; F Makino; K Makishima; A Marscher; J McEnery; IM McHardy; DI Meyer; EM Moore; E Ramos; EI Robson; HJ Rose; MS Schubnell; G Sembroski; JA Stevens; T Takahashi; M Tashiro; TC Weekes; C Wilson; J Zweerink
  ASTROPHYSICAL JOURNAL, Volume：459, Number：2, First page：L111, Last page：L111, Mar. 1996
  UNIV CHICAGO PRESS, English, Others
  DOI：https://doi.org/10.1086/309646
  DOI ID：10.1086/309646, ISSN：0004-637X, Web of Science ID：WOS:A1996TX19600017
• DETECTION OF INVERSE-COMPTON X-RAYS FROM LOBES OF THE RADIO GALAXY FORNAX-A　　　　　　　　　　　　　　　
  H KANEDA; M TASHIRO; Y IKEBE; Y ISHISAKI; H KUBO; K MAKISHIMA; T OHASHI; Y SAITO; H TABARA; T TAKAHASHI
  ASTROPHYSICAL JOURNAL, Volume：453, Number：1, First page：L13, Last page：L16, Nov. 1995
  Extended X-ray emission was detected with ASCA from the synchrotron double lobes of the radio galaxy Fornax A. This is thought to be the same emission as was detected with ROSAT. The excess X-rays exhibit very hard spectra, described by a power law of energy index 1.2 +/- 0.5. Since this index is consistent with the synchrotron. radio index of 0.9 +/- 0.2, the X-rays are thought to arise when the radio-emitting relativistic electrons make inverse-Compton scattering off the cosmic microwave photons. Comparison of the X-ray and radio fluxes yields the lobe magnetic field intensity of 2-4 mu G. The relativistic electrons in the lobes are inferred to have an energy density close to that of the magnetic fields.
  UNIV CHICAGO PRESS, English
  DOI：https://doi.org/10.1086/309742
  DOI ID：10.1086/309742, ISSN：0004-637X, Web of Science ID：WOS:A1995TB04300004
• 27p-SC-10 ASCA observation of the radio galaxy Centaurus B　　　　　　　　　　　　　　　
  Tashiro M.; Makishima K.; Kaneda H.; Ishisaki Y.; Iyomoto N.; Idesawa E.; Takahashi T.; Kotani T.; Yamashita A.
  Abstracts of the meeting of the Physical Society of Japan. Sectional meeting, Volume：1995, Number：1, First page：142, Last page：142, 12 Sep. 1995
  The Physical Society of Japan (JPS), Japanese
  CiNii Articles ID：110001981556, CiNii Books ID：AN10453836
• 27p-SC-4 In-Orbit Non X-ray Background Characteristics of ASCA GIS　　　　　　　　　　　　　　　
  Idesawa E.; Ikebe Y.; Ishisaki Y.; Ueda Y.; Kubo H.; Kohmura Y.; Takahashi T.; Tashiro M.; Makishima K.; GIS team
  Abstracts of the meeting of the Physical Society of Japan. Sectional meeting, Volume：1995, Number：1, First page：140, Last page：140, 12 Sep. 1995
  The Physical Society of Japan (JPS), Japanese
  CiNii Articles ID：110001981552, CiNii Books ID：AN10453836
• 28a-SK-8 A performance test of phototube for Hard X-ray Detector on ASTRO-E　　　　　　　　　　　　　　　
  Mizuno Tsunefumi; Fukazawa Yasushi; Saitou Yositaka; Makishima Kazuo; Takahashi Tadayuki; Kamae Tsuneyosi; Tashiro Makoto; the XHD team
  Abstracts of the meeting of the Physical Society of Japan. Sectional meeting, Volume：1995, Number：1, First page：41, Last page：41, 12 Sep. 1995
  The Physical Society of Japan (JPS), Japanese
  CiNii Articles ID：110001981382, CiNii Books ID：AN10453836
• 28a-SK-5 Development of PIN type Silicon hard X-ray detector for ASTRO-E satellite(II)　　　　　　　　　　　　　　　
  Sugizaki M; Iyomoto Y.; Tamura T.; Kaneda H.; Murakami T.; Takahashi T.; Tashiro M.; Fukazawa Y.; Makishima K.; Kamae T.; HXD Working Group
  Abstracts of the meeting of the Physical Society of Japan. Sectional meeting, Volume：1995, Number：1, First page：40, Last page：40, 12 Sep. 1995
  The Physical Society of Japan (JPS), Japanese
  CiNii Articles ID：110001981380, CiNii Books ID：AN10453836
• 28a-SK-6 Development of PIN type Silicon hard X-ray detector for ASTRO-E satellite(III)　　　　　　　　　　　　　　　
  Iyomoto N.; Sugizaki M; Tamura T.; Kaneda H.; Tashiro M.; Fukazawa Y.; Makishima K.; Kamae T.; Murakami T.; Takahashi T.; HXD Working Group
  Abstracts of the meeting of the Physical Society of Japan. Sectional meeting, Volume：1995, Number：1, First page：40, Last page：40, 12 Sep. 1995
  The Physical Society of Japan (JPS), Japanese
  CiNii Articles ID：110001981381, CiNii Books ID：AN10453836
• 27p-SC-7 Physics in the Central Region of Clusters of Galaxies as Revealed with ASCA　　　　　　　　　　　　　　　
  Makishima K; Tashiro M; Fukazawa Y; Ishisaki Y; Saito Y; Ezawa H; Kaneda H; Matsuzaki K; Matsushita K; Tamura T; Ikebe Y; Kubo H; Takahashi T; Hirayama M; Ohashi T; Kikuchi K
  Abstracts of the meeting of the Physical Society of Japan. Sectional meeting, Volume：1995, Number：1, First page：140, Last page：140, 12 Sep. 1995
  The Physical Society of Japan (JPS), Japanese
  CiNii Articles ID：110001981553, CiNii Books ID：AN10453836
• 27p-SC-9 X-rays from the "Lobes" of the radio galaxy Fornax A(II)　　　　　　　　　　　　　　　
  Kaneda H; Tashiro M; Makishima K; Ishisaki Y; Takahashi T; Kubo H; Ohashi T
  Abstracts of the meeting of the Physical Society of Japan. Sectional meeting, Volume：1995, Number：1, First page：141, Last page：141, 12 Sep. 1995
  The Physical Society of Japan (JPS), Japanese
  CiNii Articles ID：110001981555, CiNii Books ID：AN10453836
• 27p-SC-11 Observations of starburst galaxies with ASCA　　　　　　　　　　　　　　　
  Obayashi Hitoshi; Fukazawa Yasushi; Makishima Kazuo; Tashiro Makoto; Awaki Hisamitsu; Mihara Tatehiro; Ohashi Takaya; Tsuru Takaesi
  Abstracts of the meeting of the Physical Society of Japan. Sectional meeting, Volume：1995, Number：1, First page：142, Last page：142, 12 Sep. 1995
  一般社団法人日本物理学会, Japanese
  CiNii Articles ID：110001981557, CiNii Books ID：AN10453836
• ハイテクとおめがね事情(6)X線天文衛星「あすか」　　　　　　　　　　　　　　　
  田原 譲; 田代 信; 小谷 太郎
  Volume：88, Number：6, First page：264, Last page：265, Jun. 1995
  Japanese
  ISSN：0374-2466, CiNii Articles ID：10002143177, CiNii Books ID：AN00154555
• Development of X-ray Polarimeter for X-ray Astronomy(II)　　　　　　　　　　　　　　　
  Okada K.; Makishima K.; Tashiro M.; Ikebe Y.; Ishisaki Y.; Mihara T.
  Abstracts of the meeting of the Physical Society of Japan. Annual meeting, Volume：50, Number：1, First page：131, Last page：131, 16 Mar. 1995
  The Physical Society of Japan (JPS), Japanese
  CiNii Articles ID：110002132174, CiNii Books ID：AN10451127
• Study of the Galactic Ridge X-ray Emission　　　　　　　　　　　　　　　
  Kaneda H.; Makishima K.; Tashiro M.; Matsuzaki K.; Sugizaki M.; Tanaka Y.; Yamauchi S.; Yamasaki N.
  Abstracts of the meeting of the Physical Society of Japan. Annual meeting, Volume：50, Number：1, First page：132, Last page：132, 16 Mar. 1995
  The Physical Society of Japan (JPS), Japanese
  CiNii Articles ID：110002132197, CiNii Books ID：AN10451127
• Development of PIN type Silicon hard X-ray detector for ASTRO-E satellite　　　　　　　　　　　　　　　
  Tamura T.; Kaneda H.; Sugizaki M.; Tashiro M.; Makishima K.; Takahashi T.; Kamae T.; Murakami T.; HXT Working Group
  Abstracts of the meeting of the Physical Society of Japan. Annual meeting, Volume：50, Number：1, First page：33, Last page：33, 16 Mar. 1995
  The Physical Society of Japan (JPS), Japanese
  CiNii Articles ID：110002131054, CiNii Books ID：AN10451127
• X-rays from the "Lobes" of the radio galaxy Fornax A　　　　　　　　　　　　　　　
  Tashiro M; Makishima K; Kaneda H; Takahashi T; Kubo H; Ishisaki Y; Ohashi T
  Abstracts of the meeting of the Physical Society of Japan. Annual meeting, Volume：50, Number：1, First page：133, Last page：133, 16 Mar. 1995
  The Physical Society of Japan (JPS), Japanese
  CiNii Articles ID：110002132203, CiNii Books ID：AN10451127
• ASCA Observations of Low Luminosity AGN candidates　　　　　　　　　　　　　　　
  Iyomoto N; Makishima K; Fukazawa Y; Tashiro M; Ohtsuka T; Ohashi T
  Abstracts of the meeting of the Physical Society of Japan. Annual meeting, Volume：50, Number：1, First page：133, Last page：133, 16 Mar. 1995
  The Physical Society of Japan (JPS), Japanese
  CiNii Articles ID：110002132212, CiNii Books ID：AN10451127
• X-RAY-SPECTRUM OF THE BL-LACERTAE OBJECT PKS-0548-322 OBSERVED WITH GINGA　　　　　　　　　　　　　　　
  M TASHIRO; K MAKISHIMA; T OHASHI; M INDAKOIDE; A YAMASHITA; T MIHARA; Y KOHMURA
  PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN, Volume：47, Number：2, First page：131, Last page：140, 1995
  The BL Lac object PKS 0548-322 was observed in X-rays with Ginga five times between 1990 January and 1991 March. The 2-20 keV flux varied by a factor of 2.5, and the spectral energy index a showed a significant change of between 0.8+/-0.02 and 1.03+/-0.04. No simple relation has been found between the flux and the spectral index. An upper limit for the equivalent width of the iron K line is 83 eV at 90% confidence. Based on the spectral results, we propose a simple scheme to interpret the variation of the X-ray spectrum in terms of the synchrotron emission. This gives new constraints on the properties of the emission region.
  ASTRONOMICAL SOC JAPAN, English
  ISSN：0004-6264, Web of Science ID：WOS:A1995QW81400006
• ASCA OBSERVATIONS OF THE SPECTRUM OF THE X-RAY-BACKGROUND　　　　　　　　　　　　　　　
  KC GENDREAU; R MUSHOTZKY; AC FABIAN; SS HOLT; T KII; PJ SERLEMITSOS; Y OGASAKA; Y TANAKA; MW BAUTZ; Y FUKAZAWA; Y ISHISAKI; Y KOHMURA; K MAKISHIMA; M TASHIRO; Y TSUSAKA; H KUNIEDA; GR RICKER; RK VANDERSPEK
  PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN, Volume：47, Number：2, First page：L5, Last page：L9, 1995
  We present initial results from ASCA on the spectrum of the Cosmic X-ray Background from 0.4 to 10 keV. About 250 ks of deep survey data has been collected from the performance verification phase of ASCA. About 110 ks of dark-earth data are used to assess the internal background. A single power-law describes the X-ray background very well in the 1 to 10 keV with no evidence for a steepening in the 1 to 3 keV range. At 1 keV, the intensity of the X-ray background is 9.6 keV s(-1) cm(-2) sr-l keV(-1). Our data clearly show an excess above the extrapolation of the single power law model below 1 keV. At least part of this excess can be accounted for with a thermal component as there is evidence for O VII and O VIII emission.
  ASTRONOMICAL SOC JAPAN, English
  ISSN：0004-6264, Web of Science ID：WOS:A1995QW81400001
• 1a-J-11 ASCA Serendipitous Source Survey of the CXB(I)　　　　　　　　　　　　　　　
  Ishisaki Y; Kubo H; Takahashi T; Tashiro M; Ikebe Y; Makishima K; Ueda Y; Ogasaka Y; Kii T; Inoue H; Yamasaki N
  Abstracts of the meeting of the Physical Society of Japan. Sectional meeting, Volume：1994, Number：1, First page：171, Last page：171, 12 Sep. 1994
  The Physical Society of Japan (JPS), Japanese
  CiNii Articles ID：110002055663, CiNii Books ID：AN10453836
• 1a-J-12 ASCA Serendipitous Source Survey of the CXB(II)　　　　　　　　　　　　　　　
  Takahashi T; Ishisaki Y; Takahashi T; Tashiro M; Ikebe Y; Makishima K; Ueda Y; Ogasaka Y; Kii T; Inoue H; Yamasaki N
  Abstracts of the meeting of the Physical Society of Japan. Sectional meeting, Volume：1994, Number：1, First page：172, Last page：172, 12 Sep. 1994
  The Physical Society of Japan (JPS), Japanese
  CiNii Articles ID：110002055665, CiNii Books ID：AN10453836
• 1a-J-3 Development of Driftless SPC　　　　　　　　　　　　　　　
  Iyomoto N; Fukazawa Y; Tashiro M; Makishima K; Ohashi T; yamasaki N; Mutoh K
  Abstracts of the meeting of the Physical Society of Japan. Sectional meeting, Volume：1994, Number：1, First page：168, Last page：168, 12 Sep. 1994
  The Physical Society of Japan (JPS), Japanese
  CiNii Articles ID：110002055648, CiNii Books ID：AN10453836
• 1a-J-9 X-Ray Spectra from Quasars and Physical State Around the Nuclei　　　　　　　　　　　　　　　
  Tashiro M; Yamashita A; Kii T; Ohashi T; Makishima K; Iyomoto N; Idesawa E
  Abstracts of the meeting of the Physical Society of Japan. Sectional meeting, Volume：1994, Number：1, First page：170, Last page：170, 12 Sep. 1994
  The Physical Society of Japan (JPS), Japanese
  CiNii Articles ID：110002055659, CiNii Books ID：AN10453836
• 31p-YW-10 Development of X-ray Polarimeter for X-ray Astronomy　　　　　　　　　　　　　　　
  Okada K; Makishima K; Tashiro M; Ikebe Y; Ishisaki Y; Mihara T
  Abstracts of the meeting of the Physical Society of Japan. Annual meeting, Volume：49, Number：1, First page：177, Last page：177, 16 Mar. 1994
  The Physical Society of Japan (JPS), Japanese
  CiNii Articles ID：110002161564, CiNii Books ID：AN10451127
• 29a-YW-2 「あすか」に搭載されたGIS検出器の性能　　　　　　　　　　　　　　　
  大橋 隆哉; 深沢 泰司; 渡辺 靖; 石崎 欣尚; 上条 俊介; 金田 英広; 香村 芳樹; 牧島 一夫; 松下 恭子; 中川 健一郎; 田代 信; 石田 学; 井上 一; 槙野 文明; 村上 敏夫; 小笠原 嘉明; 田中 靖郎; 上田 佳宏; 三原 建弘; 竹島 敏明; 鶴 剛; 海老沢 研
  Volume：49, Number：1, First page：167, Last page：167, 16 Mar. 1994
  Japanese
  CiNii Articles ID：110002161488, CiNii Books ID：AN10451127
• 30p-YW-12 The Development of position sensitive gas scintillation proportional counter　　　　　　　　　　　　　　　
  Fukazawa Y; Nakagawa K; Tamura T; Tashiro M; Makishima K; Ohashi T; Yamazaki N
  Abstracts of the meeting of the Physical Society of Japan. Annual meeting, Volume：49, Number：1, First page：177, Last page：177, 16 Mar. 1994
  The Physical Society of Japan (JPS), Japanese
  CiNii Articles ID：110002161569, CiNii Books ID：AN10451127
• X-RAY CONTINUUM AND IRON-K EMISSION-LINE FROM THE RADIO GALAXY 3C 390.3　　　　　　　　　　　　　　　
  M INDA; K MAKISHIMA; Y KOHMURA; M TASHIRO; T OHASHI; P BARR; K HAYASHIDA; GGC PALUMBO; G TRINCHIERI; M ELVIS; G FABBIANO
  ASTROPHYSICAL JOURNAL, Volume：420, Number：1, First page：143, Last page：151, Jan. 1994
  X-ray properties of the radio galaxy 3C 390.3 were investigated using the EXOSAT and Ginga satellites. Long-term, large-amplitude X-ray intensity changes were detected over a period extending from 1984 through 1991, and high-quality X-ray spectra were obtained especially with Ginga. The X-ray continuum spectra were described with power-law model with photon slope in the range 1.5-1.8, and the slope flattened as the 2-20 keV luminosity decreased by 40%. There was a first detection of the iron emission line from this source at the 90% confidence level. An upper limit was derived on the thermal X-ray component. X-ray emission mechanisms and possible origins of the long-term variation are discussed.
  UNIV CHICAGO PRESS, English
  DOI：https://doi.org/10.1086/173547
  DOI ID：10.1086/173547, ISSN：0004-637X, Web of Science ID：WOS:A1994MN70100011
• DISCOVERY OF AN OBSCURED LOW-LUMINOSITY ACTIVE NUCLEUS IN THE SPIRAL GALAXY NGC-4258　　　　　　　　　　　　　　　
  K MAKISHIMA; R FUJIMOTO; Y ISHISAKI; T KII; M LOEWENSTEIN; R MUSHOTZKY; P SERLEMITSOS; T SONOBE; M TASHIRO; T YAQOOB
  PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN, Volume：46, Number：3, First page：L77, Last page：&, 1994
  The spectra and images of the nearby jet galaxy NGC 4258 (M106) obtained with ASCA indicate presence of several distinct X-ray emission components. The emission above 3 keV is pointlike and coincident in position with the optical nucleus, exhibiting a hard (photon index approximately 1.78) and absorbed (N(H) approximately 1.5 x 10(23) cm-2) spectrum. This provides clear evidence that NGC 4258 hosts an obscured active nucleus of low luminosity, about 4 x 10(40) ergs s-1 in 2-10 keV after removing the absorption. Iron K-line emission with an equivalent width 0.25 +/- 0.10 keV was detected. The emission below 1 keV is dominated by an extended (approximately 4') thin-thermal component with a temperature approximately 0.5 keV exhibiting atomic emission lines, possibly associated with the jet. There exists a third continuum component with an intermediate spectral hardness, which is brightest at approximately 1' south-east of the nucleus.
  ASTRONOMICAL SOC JAPAN, English
  ISSN：0004-6264, Web of Science ID：WOS:A1994NV12400008
• X-RAY VARIABILITY FROM THE BL LACERTAE OBJECT H0323+022　　　　　　　　　　　　　　　
  Y KOHMURA; K MAKISHIMA; M TASHIRO; T OHASHI; CM URRY
  PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN, Volume：46, Number：2, First page：131, Last page：138, 1994
  The BL Lacertae object H0323+022 was observed in X-rays with Ginga on three occasions, in 1987 July, 1988 August, and 1991 August. In the 1987 observation, the source was relatively bright, and variable by a factor of 3 on time scales of several hours. The observed 2-20 keV energy flux ranged between 2.2 and 4.1 x 10(-11) ergs CM-2 s-1 during the variation. The X-ray spectra were well described by a power-law model without intrinsic photoelectric absorption, and the photon index varied between 1.3 and 1.9 as the intensity changed. The spectrum was much better correlated with the time derivative of the X-ray intensity than the intensity, itself, in such a way that the spectrum hardened when the intensity increased. A detailed analysis of this spectrum-intensity correlation indicates that variation in the higher-energy band (4.1-10.5 keV) precedes that in the lower-energy band (1.2-4.1 keV) by roughly 0.05 d. This supports the idea that X-ray emission from H0323+022 is of synchrotron origin. In the 1988 and 1991 observations, the source was rather faint and only marginally detected at a 2-20 keV flux level between 0.6 and 1.1 x 10(-11) ergs CM-2 S-1. On these two occasions no intensity variations were detected, and soft spectra with a photon index of more than 2.0 are indicated.
  ASTRONOMICAL SOC JAPAN, English
  ISSN：0004-6264, Web of Science ID：WOS:A1994NH73500007
• THE X-RAY-EMISSION OF 3C-273 OBSERVED WITH ASCA　　　　　　　　　　　　　　　
  T YAQOOB; P SERLEMITSOS; R MUSHOTZKY; G RICKER; J WOO; K WEAVER; T KII; K MITSUDA; T KOTANI; K HAYASHIDA; S MURAKAMI; M TASHIRO
  PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN, Volume：46, Number：3, First page：L49, Last page：L53, 1994
  We report preliminary results of an ASCA observation of 3C 273. There is no spectral variability within the ASCA observation, in contrast to the longer term behavior found with EXOSAT and Ginga which established significant changes in the spectral index of the power-law continuum on timescales of a week or more, uncorrelated with luminosity. Comparison of the ASCA data with a simultaneous ROSAT/Ginga observation in 1990 December shows that while the shape of the spectrum above approximately 1 keV is essentially the same, the flux in the soft component, below approximately 1 keV, is considerably weaker relative to the hard component in the ASCA observation. The 2-10 keV luminosity is at least a factor of approximately 1.5 greater in the ASCA observation than in the ROSAT/Ginga observation whilst the ratio of 2-10 keV luminosity to 0.4-1.0 keV luminosity increases by a factor of approximately 1.2. Thus the spectral shape of the hard component appears to be independent of the relative magnitude of the soft component and is an important constraint on emission and reprocessing models. We find no significant Fe K line-emission in this observation. The data also highlight very well some of the outstanding problems in the instrumental responses.
  ASTRONOMICAL SOC JAPAN, English
  ISSN：0004-6264, Web of Science ID：WOS:A1994NV12400003
• X-RAY-PROPERTIES OF ACTIVE GALAXIES WITH HIGH INTRINSIC ABSORPTION　　　　　　　　　　　　　　　
  RS WARWICK; S SEMBAY; T YAQOOB; K MAKISHIMA; T OHASHI; M TASHIRO; Y KOHMURA
  MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY, Volume：265, Number：2, First page：412, Last page：420, Nov. 1993
  We present the results of Ginga observations of three narrow emission line X-ray galaxies, NGC 7172, NGC 7582 and ESO 103-G35. In each of these galaxies the column density along the line of sight to the active nucleus is extremely high (i.e. n(H) greater-than-or-similar-to 10(23) cm-2). A comparison of the optical depth in the iron K-edge with the low-energy absorption in the X-ray spectrum indicates an apparent iron abundance in excess of the solar value in these sources. Measurements of the iron K-edge energy show that the bulk of the X-ray-absorbing gas is not strongly photoionized, with only ESO 103-G35 exhibiting an edge energy significantly above that for neutral iron. In the case of NGC7582, the line-of-sight column density may have increased by a factor of approximately 3 over an interval of about 4 yr. The implications of these results for current models of the state and distribution of gaseous material in low-luminosity active galactic nuclei are briefly discussed.
  BLACKWELL SCIENCE LTD, English
  ISSN：0035-8711, Web of Science ID：WOS:A1993MF85400017
• THE X-RAY SPECTRAL VARIABILITY OF THE BL LACERTAE TYPE OBJECT PKS-2155-304　　　　　　　　　　　　　　　
  S SEMBAY; RS WARWICK; CM URRY; J SOKOLOSKI; IM GEORGE; F MAKINO; T OHASHI; M TASHIRO
  ASTROPHYSICAL JOURNAL, Volume：404, Number：1, First page：112, Last page：123, Feb. 1993
  We present a detailed study of the hard X-ray properties of the BL Lacertae object PKS 2155-304 based on measurements made in 1988 and 1989 with the Large Area Counter (LAC) on board the Ginga satellite. The source exhibited a high degree of variability with a dynamic range of a factor 7 in the 2-6 keV band. The fastest amplitude variation was a factor 2 decline in the intensity in this band within 4 hours. The spectrum is characterized by a break which occurs at approximately 4 keV. Spectral fits to the data integrated in 6400 s time bins reveal that, in common with previous observations of BL Lacertae objects, the spectral slope is generally anticorrelated with intensity in the sense that the spectrum hardens as the intensity increases. However, the tracks of sequential points in the index-intensity plane are occasionally seen to differ during the rise and decay stages of individual flares. Furthermore, during one, or possibly two, flaring episodes the spectral index is observed to correlate with intensity variations. The X-ray properties of PKS 2155-304 are most readily interpreted in terms of direct synchrotron radiation originating within a relativistic jet, however, the X-ray emitting region is probably more complex than the geometries assumed in most standard jet models. Further development of time-dependent theoretical models will be necessary to explain some of the details of the present observations.
  UNIV CHICAGO PRESS, English
  DOI：https://doi.org/10.1086/172263
  DOI ID：10.1086/172263, ISSN：0004-637X, Web of Science ID：WOS:A1993KK91200011
• X-RAY-SPECTRA OF BRIGHT CORE-DOMINANT QUASARS - NRAO-140 AND 4C-34.47　　　　　　　　　　　　　　　
  T OHASHI; M TASHIRO; K MAKISHIMA; T KII; F MAKINO; MJL TURNER; OR WILLIAMS
  ASTROPHYSICAL JOURNAL, Volume：398, Number：1, First page：87, Last page：93, Oct. 1992
  Two bright quasars NRAO 140 (z = 1.258) and 4C 34.47 (z = 0.206) have been studied with Ginga. The observed spectra in the energy range 2-20 keV, in the observer rest frame, are well described by power-law models. The measured 2-10 keV luminosities and energy indices are L(x) = 3.8 x 10(46) ergs s-1 and alpha = 0.72 +/- 0.11 for NRAO 140, and L(x) = 5.3 x 10(44) ergs s-1 and alpha = 0.64(-0.14)+0.17 for 4C 34.47 (H-0 = 100 km s-1 Mpc-1; q0 = 0.5); the intensity variation was less than about 10% during the approximately 1 day observation for each source. Upper limits, in the source rest frame, for iron line emission are EW < 200 and EW < 120 eV for NRAO 140 and 4C 34.47, respectively. The featureless X-ray spectra, whose slopes are flatter than those of BL Lac objects, and the high X-ray luminosities in excess of the extension of the IR-optical continuum are consistent with the synchrotron self-Compton emission accompanied by a moderate beaming toward us.
  UNIV CHICAGO PRESS, English
  DOI：https://doi.org/10.1086/171838
  DOI ID：10.1086/171838, ISSN：0004-637X, Web of Science ID：WOS:A1992JQ39700009
• 4a-G-12 ASTRO-D衛星搭載用GISの開発I　　　　　　　　　　　　　　　
  牧島 一夫; 大橋 隆哉; 田代 信; 香村 芳樹; 池辺 靖; 浅沼 達彦; 石崎 欣尚; 深沢 泰司; 井上 一; 石田 学; 上田 佳宏; 村上 敏夫; 田中 靖郎; 鶴 剛; 三原 建弘; 竹島 敏明; 海老沢 研
  Volume：1992, Number：1, First page：147, Last page：147, 14 Sep. 1992
  Japanese
  CiNii Articles ID：110001998360, CiNii Books ID：AA11823236
• ASTRO‐D衛星搭載用GISの開発 II
  大橋隆哉; 牧島一夫; 田代信; 井上一; 石田学; 鶴剛; 三原建弘; 竹島敏明; 海老沢研
  日本物理学会講演概要集(分科会), Volume：1992, Number：Autumn Pt 1, First page：147, Sep. 1992
  Japanese
  J-Global ID：200902092065388700
• ASTRO‐D衛星搭載用GISの開発 I
  牧島一夫; 大橋隆哉; 田代信; 深沢泰司; 井上一; 田中靖郎; 鶴剛; 三原建弘; 海老沢研
  日本物理学会講演概要集(分科会), Volume：1992, Number：Autumn Pt 1, First page：147, Sep. 1992
  Japanese
  J-Global ID：200902098976611537
• ASTRO‐D搭載用GIS装置の開発
  三原建弘; 大橋隆哉; 牧島一夫; 鶴剛; 石田学; 田代信; 香村芳樹; 池辺靖; 井上一
  科学衛星シンポジウム, Volume：1991, First page：23, Last page：28, Oct. 1991
  Japanese
  J-Global ID：200902076306355650
• NONPERIODIC INTENSITY VARIATIONS IN THE X-RAY PULSAR GX301-2　　　　　　　　　　　　　　　
  M TASHIRO; K MAKISHIMA; T OHASHI; T SAKAO; AE SANSOM
  MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY, Volume：252, Number：1, First page：156, Last page：162, Sep. 1991
  Ginga observations of the X-ray binary pulsar GX301 - 2 are analysed for their temporal and spectral properties. We report the unambiguous detection of aperiodic intensity variations of 7-10 per cent rms relative amplitude over time-scales covering approximately 16 to 0.1 s. These variations are self-similar, being well fitted by a power law in power spectral density versus frequency space. The pulse period measured is 689.80 s, the shortest yet measured for this source. The fraction of X-rays which is pulsed is energy dependent, being greater at higher energies. The fractional aperiodic variability shows no such energy dependence, nor do they appear to be significantly dependent on source intensity, pulse phase or absorbing column measured. These facts strongly suggest that the aperiodic variations are not caused by absorption variations, but are intrinsic to the source. The iron-line intensity shows little pulsations, but surprisingly shows significant aperiodic variability down to a time-scale as short as several seconds, thus giving a constraint to the size of the line emission region.
  BLACKWELL SCIENCE LTD, English
  ISSN：0035-8711, Web of Science ID：WOS:A1991GE36800018
• NONPERIODIC INTENSITY VARIATIONS IN THE X-RAY PULSAR GX301-2　　　　　　　　　　　　　　　
  M TASHIRO; K MAKISHIMA; T OHASHI; T SAKAO; AE SANSOM
  MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY, Volume：252, Number：1, First page：156, Last page：162, Sep. 1991
  Ginga observations of the X-ray binary pulsar GX301 - 2 are analysed for their temporal and spectral properties. We report the unambiguous detection of aperiodic intensity variations of 7-10 per cent rms relative amplitude over time-scales covering approximately 16 to 0.1 s. These variations are self-similar, being well fitted by a power law in power spectral density versus frequency space. The pulse period measured is 689.80 s, the shortest yet measured for this source. The fraction of X-rays which is pulsed is energy dependent, being greater at higher energies. The fractional aperiodic variability shows no such energy dependence, nor do they appear to be significantly dependent on source intensity, pulse phase or absorbing column measured. These facts strongly suggest that the aperiodic variations are not caused by absorption variations, but are intrinsic to the source. The iron-line intensity shows little pulsations, but surprisingly shows significant aperiodic variability down to a time-scale as short as several seconds, thus giving a constraint to the size of the line emission region.
  BLACKWELL SCIENCE LTD, English
  ISSN：0035-8711, Web of Science ID：WOS:A1991GE36800018
• 27p-SC-8 The Gas Imaging Scintillation Proportional Counter on Astro-D Mission　　　　　　　　　　　　　　　
  Koumura Yoshiki; Makishima Kazuo; Ohashi Takaya; Ishida Manabu; Tsuru Takeshi; Tashiro Makoto; Mihara Tatehiro; Kamijo Shunsuke; Ikebe Yasushi; Inoue Hajime
  春の分科会講演予稿集, Volume：1991, Number：1, First page：81, Last page：81, 11 Mar. 1991
  一般社団法人日本物理学会, Japanese
  CiNii Articles ID：110001903622, CiNii Books ID：AA11403638
• Development of imaging type fluorescence proportional counter (IGSPC).
  大橋隆哉; 牧島一夫; 鶴剛; 石田学; 三原建弘; 田代信; 香村芳樹; 井上一
  搭載機器基礎開発成果報告書, Volume：4, First page：1, Last page：5, Mar. 1991
  Japanese
  J-Global ID：200902031347213874
• Focal plane detector GIS for ASTRO-D.
  鶴剛; 大橋隆哉; 牧島一夫; 石田学; 田代信; 三原建弘; 井上一
  科学衛星シンポジウム, Volume：1990, First page：43, Last page：46, Dec. 1990
  Japanese
  J-Global ID：200902049987733366
• DISCOVERY OF A PROMINENT CYCLOTRON ABSORPTION FEATURE FROM THE TRANSIENT-X-RAY PULSAR X0331+53　　　　　　　　　　　　　　　
  K MAKISHIMA; T MIHARA; M ISHIDA; T OHASHI; T SAKAO; M TASHIRO; T TSURU; T KII; F MAKINO; T MURAKAMI; F NAGASE; Y TANAKA; H KUNIEDA; Y TAWARA; S KITAMOTO; S MIYAMOTO; A YOSHIDA; MJL TURNER
  ASTROPHYSICAL JOURNAL, Volume：365, Number：2, First page：L59, Last page：L62, Dec. 1990
  UNIV CHICAGO PRESS, English
  DOI：https://doi.org/10.1086/185888
  DOI ID：10.1086/185888, ISSN：0004-637X, Web of Science ID：WOS:A1990EL77400005
• NEW OBSERVATIONS OF THE CYCLOTRON ABSORPTION FEATURE IN HERCULES-X-1　　　　　　　　　　　　　　　
  T MIHARA; K MAKISHIMA; T OHASHI; T SAKAO; M TASHIRO; F NAGASE; Y TANAKA; S KITAMOTO; S MIYAMOTO; JE DEETER; PE BOYNTON
  NATURE, Volume：346, Number：6281, First page：250, Last page：252, Jul. 1990
  MACMILLAN MAGAZINES LTD, English
  DOI：https://doi.org/10.1038/346250a0
  DOI ID：10.1038/346250a0, ISSN：0028-0836, CiNii Articles ID：80005358368, Web of Science ID：WOS:A1990DP45600056
• X-ray Pulsars and Magnetic Fields of Neutron Stars　　　　　　　　　　　　　　　
  MAKISHIMA K; SAKAO T; MIHARA T; TASHIRO M; ISHIDA M; OHASHI T; NAGASE F; MURAKAMI T; TANAKA Y; YOSHIDA A
  Volume：25, First page：195, Last page：204, Jan. 1990
  Observations of a cyclotron absorption feature in the spectrum of X-ray pulsars are reported. The cyclotron absorption features have been discovered with Ginga in two X-ray pulsars, 4U 1538-52 (at 21keV) and X0331+53 (at 28keV). Ginga data indicate that the known cyclotron feature in the spectrum from Her X-1 should be regarded as an absorption feature at &acd;34keV rather than an emission feature at &acd;50keV. These results indicate that he cyclotron absorption feature should be common in binary X-ray pulsars. We infer that the high-energy spectral break, characteristic of X-ray pulsars, is a direct consequence of the cyclotron resonance, and closely related to the absorption feature. This implies that the spectral break, instead of the absorption feature, can be used as a convenient measure of the field strength for many X-ray pulsars. It is suggested that the X-ray pulsars exhibit a rather narrow scatter in the field strength, namely in the range of (1-4)×10^<12> G.
  Japan Aerospace Exploration Agency, Japanese
  ISSN：0285-9920, CiNii Articles ID：110000222875, CiNii Books ID：AN00354485
• 理学部研究ニュース　　　　　　　　　　　　　　　
  森沢 正昭; 神部 勉; 牧島 一夫; 大橋 隆哉; 石田 学; 坂尾 太郎; 鶴 剛; 田代 信; 三原 建弘; 印田 美香; 好村 芳樹; 米倉 伸之; 高尾 英行; 十倉 好紀; 石原 正泰; 江口 徹; 守 隆夫; 長澤 弘; 東江 昭夫; 増田; 白田 由香利; 國井 利泰; Krishman Deepa; 川島 誠一郎; 渡辺 嘉久; 尾本 恵市; 伊藤 谷生; ゲラー R; 金森 審子; 北品 健; 井上 康男; 永嶺 譲忠; 山崎 敏光; 飯島 健
  Volume：21, Number：3, First page：21, Last page：25, Dec. 1989
  Japanese
  CiNii Articles ID：120001631158, CiNii Books ID：AA11686521